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The Boston Globe | January 2, 2013
By Kiran Gupta
One busy call night, while handling multiple admissions from our emergency room, I received a page notifying me that a new patient, Mr. T, had just arrived on the hospital floor. I looked up his medical record number, but no records were found in our computer system. I rushed to his room, expecting the worst.
When I arrived, he appeared remarkably stable. The chart at his bedside provided a working diagnosis for Mr. T's primary complaint, shortness of breath, but I wanted to hear directly from him about his condition. After reviewing his vital signs, I put down my notes, pulled a chair up, and began taking his history.
I started with the open-ended, "Tell me what brought you to the hospital today." Mr. T was articulate, his account rich with nuance and detail, exactly as I had hoped. I could see that he wanted to continue. I didn't interrupt. As his history unfolded, the story it told – without fancy imaging, expensive bloodwork, or invasive tests – confirmed his diagnosis. When Mr. T had answered the last of my questions, and as I made my way through each step of the physical exam, I kept thinking about his history. I could hear the murmur in his heart loud and clear, perhaps because I knew what to listen for even before I had placed the stethoscope on his chest.
I had been in his room for less than half an hour, but we had built a rapport. Mr. T had shared with me some of the most intimate details of his life. The act of taking his history had provided me with valuable information about his medical condition. Just as importantly, it offered a glimpse into how his ailment was affecting him, leaving me with a sense of empathy that I could not have gained from perusing his chart.
Though it should seem routine, my interaction with Mr. T felt like a rarity. Contrary to what I had learned in medical school, as a resident I quickly realized that in the hospital setting, a patient's history is almost never taken in logical or linear fashion, with the patient relaying a sequential series of events to a doctor seated next to him. Rather, it is often pieced together haphazardly from notes in the existing electronic medical record, old test results, and emergency room assessments — often before we even meet the patient. Time at a patient's bedside is largely spent confirming details already acquired, performing the physical exam, and ensuring that nothing was missed.
This has significant implications for the quality of care we deliver. It means that certain vital information is not always confirmed firsthand. It can be tempting to cut and paste a long oncologic history from an old clinic visit or take the medication list from a primary care doctor's note, instead of taking the time to confirm this information directly with our patients, their family, or a local pharmacy, especially in the middle of the night or on a busy day. Yet we make vital decisions based upon the accuracy of this information.
It is unrealistic to expect that all patients will understand the conditions they have been diagnosed with, or be able to relay their history using appropriate medical terminology. Dementia, infection, and many other medical and non-medical factors can significantly limit the ability of patients to provide a precise medical history. In these situations, we are forced to rely more on the physical exam, laboratory studies, whatever records we have available to us, and family members if they are present. But we have gotten into the habit of doing this so often that sometimes we forget that, when possible, we should always try to ask our patients for their medical history directly, even if they can't provide all the details. An inaccurate or cursory history can lead to a delay in diagnosis, unnecessary testing, improper medical management, or worse — harm to our patients.
Taking a patient's history properly is important not only for providing optimal medical care, but also for helping us as providers find meaning in the relationships we build with our patients. On paper, Mr. T's history was relatively similar to the story he told me as I sat by his bedside. It would certainly have taken less time to read a note from his doctor. But, the photocopied pages faxed over from a physician's office wouldn't have captured the distress in his voice as he relayed how difficult it had become to walk his dog or take a shower because of his shortness of breath – and his deep-seated worry that he would never get better.
I sense that my generation of physicians is losing something precious, the very reason why many of us were drawn to medicine in the first place — time with our patients. In a system burdened with financial pressures as well as significant time and resource constraints, it can be easy to reduce patients to charts, labs, and a list of "to dos." Yet caring for patients involves something more: It requires a sense of humanity. If we are to maintain this, we must find a way to change the current system so that we always have time to listen.


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One can still see why flatlanders started pouring into the Cashiers-Highlands region after the Civil War. The scenic ridge, valley and gorge country here remains one of the most interesting areas in Western North Carolina to explore.
Some of the most exciting spots in Panthertown Valley, Blue Valley, Whiteside Cove, and the gorge systems formed by the Horsepasture, Whitewater, and other rivers can be somewhat difficult to access. Others, however, can be reached in a matter of minutes. One such is Satulah Mountain, which is located within several miles of downtown Highlands.
Atop Satulah (elevation 4,543 feet) there are panoramic views of the North Carolina mountains surrounding the Highlands plateau. Back to the northeast there's a splendid bird's eye view of the Whiteside Mountain cliffs, while out to the west the ridges of the Nantahala range flow northward toward the Great Smokies. On a clear day, one can discern the shimmering outlines of the lake systems in South Carolina.
Satulah is classified as a heath bald since most of the mountain top is covered with a dense — in places impenetrable — cover of heath shrubs (primarily rhododendron and laurel) as well as stunted white oak, chinquapin, and witchhazel. Foot trails cut through the tangle allow one to explore the inner-workings of the habitat.
The potholes in the rock surface are said to be evidence of a fire tower that once stood on the summit. If so, one can only envy the folks who manned the tower in such an idyllic setting.
Botanically, the rock portion of the bald and adjacent cliffs are quite interesting, providing one of the best examples of this type of summit habitat. Here one can find mats of twisted haircap moss (really a clubmoss relative rather than a moss), one of the few stands of mountain juniper in North Carolina, and sand myrtle.
In an informative book titled High Lands (1964), T.W. Reynolds stated that the mountain was "sometimes affectionately called Stooly by the natives, and spelled Stuly in the old town minutes." Reynolds made a lengthy, convoluted, and unconvincing argument as to how the name "Satulah" may derive from the Cherokee word for "Six Killer."
Satulah is one of those places in the North Carolina mountains associated with strange quakes, tremors, and smoke. In the late 1800s, Bureau of American Ethnology worker James Mooney collected data on sites where it was thought "volcanic activity ... left traces in the Carolina mountains." Mooney cited areas in Madison and Rutherford counties where warm springs issued forth while peaks "rumbled and smoked." He was told by locals that a mountain in Haywood County near the head of Fines Creek suffered an explosion that "split solid masses of granite as though by a blast of gunpowder." In Cherokee County, a violent earthquake was thought to have "left a chasm extending for several hundred yards, which is still to be seen."
As to Satulah (which Mooney spelled "Satoola"), the crevices on the sides of the mountain were said from time to time to issue forth smoke. Mrs. Ed Picklesimer, a resident of the Clear Creek community below Satulah, told Reynolds that, "years ago she saw smoke and light there." If one looks through the older literature about the WNC backcountry, the occurrence of so-called "smoking mountains" is rather frequent. John P. Arthur, for instance, in his History of North Carolina (1913) located a "smoker" at the head of Bee Creek in Buncombe County.
I will note that on certain days one can view the west-facing cliffs of Satulah from Little Scaly Mountain on N.C. 106 and see "smoke" curling up out of the crevices as if the inner mountain were afire. The "smoke" is in reality, however, the mist rising out of the Clear Creek Valley that is being carried into and over Satulah by eastward winds.
Even if Satulah Mountain isn't active in a volcanic sense, it's still a wonderful place to visit and enjoy. For online directions and additional information regarding access see: www.highlandhiker.com/Satulah_Mountain.html and www.colonialpinesinn.com/attractions.htm

subset: commoncrawl


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Skip Bins Gold Coast Region
Welcome to Skip Bins Gold Coast, supplier of
Skip Bins Hire and Mini Skip Bins Rental - Gold Coast
Our Skip Bins Gold Coast region service is a Queensland owned and locally operated Gold Coast area waste disposal business that has an excellent reputation for high standards of service and fast skip bin deliveries. With 5 years experience, Skip Bins Gold Coast is the best mini skip rental business on the Gold Coast providing prompt and professional waste management services with a wide range of bin sizes to suit your needs. No matter what type of job, no matter how small or large Skip Bins Gold Coast can handle it. We pride ourselves on completing your waste disposal jobs on time with customer satisfaction as our number one focus. If you need fast and reliable miniskips, then look no further than our Skip Bins Gold Coast area service.
Our skip bin hire Gold Coast region services include:
- Commercial bin, mini skip and skip bin hire.
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- Green or garden waste skip bin delivery.
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- Skip bins with doors (great for wheelbarrow access).
Gold Coast mini-skip bin hire prices
Skip Bins Gold Coast offers no-obligation, free quotes on all jobs. Give Skip Bins Gold Coast a call anytime on 0402 044 972 or fill out the form on our Contact Us page and we'll send you a quote within 24 hours. The friendly and experienced team at Skip Bins Gold Coast are ready to assist you with your enquiry and we won't let you down.
Our skip bin quotes are totally obligation-free and best of all, there are zero hidden surcharges when you deal with Skip Bins Gold Coast. Our skip bin prices include all delivery and pick up charges and dump fees.
Our team is very keen to secure your business and show you how great and dependable our service is. As such we invite you to contact our competitors for a skip bin quote, then call us. We will make sure that you are getting the best deal possible with service that you can rely on.
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At Skip Bins Gold Coast we put our customers first and give them flexible options for skip bin hire to suit all needs. Our Gold Coast skip bin rental customers can request after-hours skip bin delivery and removal, and can either simply call us when their skip is full, or schedule drop-off and/or removal.
Skip Bins Gold Coast practices safe waste transportation
Skip Bins Gold Coast cares about the well-being of other road users, our clients and our employees. This is why we make sure we understand and adhere to council regulations. Where possible we pass advice onto our customers regarding where skip bins can and can't be placed, including what can and can't be disposed of and transported in skip bins. This means Skip Bins Gold Coast always provides accurate advice to make sure you have a hassle-free experience when it comes to getting rid of unwanted waste.
The Skip Bins Gold Coast team
With customer satisfaction as our number one priority, we make sure each and every mini skip hire job is completed to the highest professional and safety standards. Our team members hold all necessary qualifications and tickets. Our equipment is modern and fully maintained operated by a team with over 5 years of collective experience.
Skip Bins Gold Coast provides Gold Coast skip bin hire services to a range of industries including housing development, construction, and commercial. We also provide residential mini skip bin hire services to the general public across the Gold Coast and Brisbane South. We take pride in our reputation as a trusted, customer-focused and professional Gold Coast skip bin hire services. We are more than happy to provide references from our other satisfied customers so you know you're hiring the best Gold Coast mini skip bin supplier.
Gold Coast skip bin hire - We look forward to assisting with your mini skip bin rental
At Skip Bins Gold Coast we deliver professional and affordable skip bin hire for anyone on the Gold Coast and into Brisbane South. No matter the size of your commercial, residential or construction waste disposal or waste management job in Coomera, Skip Bins Gold Coast has the equipment, expertise and experience to get it done on time with a focus on your satisfaction.
Looking for cost-effective, professional, hassle-free skip bin rental on the Gold Coast? We provide daily and urgent Gold Coast mini skip bin rentals all over the coast and Brisbane South, so call or text Skip Bins Gold Coast today on 0402 044 972 or send us your online booking request or online enquiry.
Frequently Asked Questions about Gold Coast skip bin hire
Yes! We pride ourselves on meeting client expectations and providing urgent skip bin deliveries. Our team are ready to spring into action if another skip bin supplier has let you down or if you just need a mini skip bin urgently.
A skip bin can only be placed where council regulations allow, and it is your responsibility to gain the necessary permit from your local council before you book a skip bin. There are different rules for different council areas to be aware of too. Don't worry, we can often work out another solution if you're denied a council permit.
You don't need any special permissions or any permits if the skip bin will be placed on your rented or mortgaged property. For delivery purposes, please allow 1m2 around the bin for placement.
You'll need to submit an application via Queensland Police in order for us to legally place a skip bin on any road.
As long as utility pits or pedestrian access won't be blocked, then generally, yes. Depending on the council area you live in, you may need a permit before we can place a skip bin on the footpath.
Our bins are meant for certain types of waste. If you don't follow certain policies, we may be charged an additional fee on arrival at a council tip (which is passed onto the customer) or find yourself in breach of weight restrictions on what a truck can lift and carry. As a general rule, any food or container that has contained chemicals or wet paint are prohibited.
• Garden waste – for example shrubbery, lawn clippings.
• Household appliances & Furniture – for example fridges, lounges, washers, dryers.
• Light building waste – for example dry timber and gyprock.
• Heavy building materials – for example concrete, asphalt, tiling and bricks.
Not Allowed:
• Insulation.
• Asbestos.
• Gas bottles.
• Tree stumps.
• Liquids.
• Oils.
• Food scraps.
• Chemical waste in solid, liquid or powder form (including garden and household chemicals).
• Containers that have been used to store wet paint or chemicals.
If you're not sure if we can remove your waste or not, our team are happy to help! Call us on 0402 044 972, seven days a week.
Please work with us regarding adherence to these regulations, as unfortunately if these materials are found in the skip bin then we will not be able to collect it until they have been removed from the bin.
Heavy materials are made of (or include) these materials or products: asphalt, concreting, brick, pavers or roof/ceramic tiles. Some equipment or larger machinery may exceed the permitted weight.
The bin must only be filled to the top so that it is level with the side of the bin. Due to occupational health and safety laws, waste cannot exceed the height of the bin as it becomes hazardous to transport to the transfer station.
If your bin is overloaded, you may be required to offload some of the contents before it can be removed from site. If you can't or don't do this, then unfortunately an additional fee of up to $100 may apply, as we will have to empty excessive contents into another skip bin before transporting both bins to the transfer station.
The appropriate bin size depends on what you're putting in. If you're a fan of the TV show "The Block" and want to conduct a Kitchen Week or Bathroom Week of your own in Coomera, a 4 cubic metre bin is the biggest you'll need. If you're doing an entire season of The Block then for the disposal of heavy materials you will need bigger bins. Or maybe you should just go on the show…feel free to send us a commission if you win for this life-changing tip!
You can check with us by sending a text message to Andrew for extra guidance on what will fit and any possible weight restrictions. You can learn more about our bin sizes by reading our skip bins page.
What's tricky is that the required area depends on the shape and size of the debris you need gone. If you work out length (metres) x width (metres) x depth (metres) x 2, that gives you the most accurate indication.
For example: 6m x 3m x 0.1m = 1.8 cubic metres (if the waste was solid) x2 = 3.6 cubic metres of required bin space.
It's also important to remember that other factors need to be considered such as lifting and carrying limits, basic safety and road rules. Also, there are certain procedures to be followed in order to transport heavy materials safely. If in doubt, just contact our team to make sure you're getting the right size and type of bin.
The minimum billable time for skip bin hire that most companies stick to is a week, as this is the industry-standard rental minimum. However, one of the great advantages of choosing Skip Bins Gold Coast is that you can hire bins out for as short as just ONE day. We are very competitive with our prices as well and we love the chance to provide a better price than our competitors. So contact the rest, then call the best.
You can hire our bins for between one and seven calendar days. For example, if you chose a seven-day hire period, and you got the bin delivered on a Monday, we'd pick it up the following Monday, unless you extend the hire period by purchasing extra days.
That's completely fine, we have many customers who do this. Just call our team on 0402 044 972 and we'll quote you.
Not at all. We're happy to organise credit card payments over the phone when ordering. Alternatively, you can arrange cash or EFTPOS payment or credit cards, (Visa or Mastercard) onsite when we drop off the skip bin. Just call our friendly team on 0402 044 972 and they will be happy to help you.
For commercial or construction companies, we are happy to establish a trade account for you and provide an invoice (payment terms are 7 days). Payment terms could be negotiated upon completion of a credit application.
It's best to book 24 hours (at least) in advance. However, we can often provide same-day delivery depending on traffic conditions and / or unforeseen delays and other bookings we have in place.
Note – Actual dimensions of each bin may vary slightly due to using different manufacturers
Unfortunately, Skip Bins Gold Coast does not allow asbestos to be disposed of in our bins. This is because asbestos is toxic and only licensed operators can remove it safely.
While the material is dangerous, homeowners are still allowed to remove 10m2 of non-friable asbestos themselves. Have a read of the Queensland Government resources to find out more.


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How to Save Brunch Calories
Cut Brunch Calories Without Feeling Deprived
Who can resist cutting into a stack of fluffy pancakes dripping with melted butter and syrup, or biting into a savory egg and sausage bagel sandwich? Weekends just don't seem the same without indulging in one of these decadent brunch favorites, except when you start to realize it's working against your best healthy efforts. You can still enjoy brunch without busting your waistline; here are some ways to save calories without feeling like you're missing out.
What you crave: French toast with maple syrup (two pieces): 498 calories
Eat this instead: Mixed berry pancakes with maple Greek yogurt (three pancakes): 288 calories
Calories saved: 210
What you crave: Eggs Benedict with hash browns: 810 calories
Eat this instead: Vegan eggs Benedict with sweet potato hash: 621
Calories saved: 189
What you crave: Egg and sausage on a bagel: 551 calories
Eat this instead: Egg and sausage on an English muffin: 392 calories
Calories saved: 159
What you crave: Cheese omelet (three eggs) with hash browns: 536 calories
Eat this instead: Scrambled eggs (two eggs) with hash browns: 350 calories
Calories saved: 186
Keeping reading for more ways to save brunch calories.
What you crave: Scrambled eggs (two eggs), bacon (three strips), hash browns, and whole-wheat toast: 588 calories
Eat this instead: Scrambled eggs (two eggs), bacon (two strips), and hash browns: 442 calories
Calories saved: 146
What you crave: Belgium waffle with whipped cream and syrup: 647 calories
Eat this instead: Belgium waffle with fresh fruit: 474 calories
Calories saved: 173
What you crave: Blueberry scone: 460 calories
Eat this instead: Chia seed blueberry muffins (two): 212 calories
Calories saved: 248


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LEWISTON, Idaho - (Box Score) With the game tied 3-3 in the bottom of the ninth, LSU Shreveport's (La) Devin Greco ended it quickly with a walk-off grand slam to propel the top-seeded Pilots to a 7-3 victory over No. 6 Lewis-Clark State (Idaho) in game 10 of the 2012 Avista-NAIA World Series at Harris Field.
With the win, the Pilots avoid becoming the first No. 1 seed since seeding began in 2003 to go 0-2. LSU Shreveport advances to play the loser of No. 2 Lee (Tenn.) and No. 3 Oklahoma City at 3 p.m. PDT on Tuesday. Lewis-Clark ends its season with a 42-14 record, including a 1-2 mark in the postseason. The Warriors have now gone 1-2 in their last four World Series appearances.
Ridge Gonsoulin and Kyle Pearson, who homered in the seventh to tie the game, set the stage with back-to-back hits to open the Pilot half of the ninth. An intentional walk of Greg Friesen loaded the bases with no outs when Greco stepped to the plate. Greco wasted no time, depositing the first pitch into the left field bleachers to give LSU Shreveport its first win in this year's World Series.
Greco was one of four Pilots with two hits on the afternoon. The other three individuals were Pearson, Friesen and Manny Estrada. As a team, LSU Shreveport tallied 12 hits, including the two previously mentioned home runs.
Jake Knight was credited with the victory for the Pilots, improving to 4-0 on the season. He scattered two hits and allowed no runs in two innings of relief. LSU Shreveport starter Matt Lackie finished with a no-decision. Lackie tossed seven innings, allowing three runs (all earned), one walk and striking out four.
Lewis-Clark State reliever Mitchell Wilhite (2-2) took the loss. He surrendered five runs (all earned) on five hits in 2.2 innings of work.
The Warriors drew first blood in the second when Jordan Payne singled down the left field line, scoring pinch runner Zach Holley and Connor Moore, who reached earlier on a walk and hit-by-pitch. Lewis-Clark added what proved to be its final run of the contest two innings later when Moore singled to give the Warriors a 3-0 lead after four.
LSU Shreveport, who only had three hits through the first five innings, pulled within one behind a two-run sixth. Greco opened the frame with a one-out double. Greco's pinch runner Cody Causey came around to score four pitches later as Estrada shot a single through the hole at short stop. Another Pilot single on a hit-and-run plated Estrada to make it 3-2.
The Pilots knotted to game on Pearson's seventh inning blast before Greco walked off in the ninth.
Seven different Warriors recorded hits in the contest.


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There's been a running narrative in the comments this season that I've focused too much attention on Michael Scott as a character, but I'd argue that was entirely warranted: This season was almost exclusively focused around Michael's inevitable departure, which meant that "Goodbye, Michael" felt like the end of the season — and, one would argue, the series — rather than its twenty-first episode.
But now we've reached the point where we are being asked to forget about Michael Scott: Steve Carell has been erased from the credits, replaced temporarily by Deangelo and what appears to be some sort of Southwest-inspired figurine, and Michael's name is never mentioned. Instead, "The Inner Circle" jumps right into the post-Michael office, exploring the new power dynamics and continuing the kinds of storylines we saw back in "Training Day" (where all the employees were doing their best to impress the new boss).
I would argue that "The Inner Circle" is more successful than that episode on some levels, mainly because it differentiates how the employees respond to Deangelo as a character. Deangelo's fake juggling act is perhaps the most telling scene here, as you can tell who is honestly impressed (Kevin, Erin), who is forcing themselves to be impressed for the sake of remaining in the Inner Circle (Jim, Darrell, Gabe), and who is completely convinced that he is nothing but a fraud (pretty much everyone else). Back in "Training Day," it seemed like everyone was ignoring the character's shtick in favor of fawning over him, and I admittedly felt that more of them would immediately shift to the position they take here.
However, both episodes suffer from the same problem: They're simply not very funny or meaningful, which I'd argue is even more problematic for "The Inner Circle" given its position in the season. While the opening of the episode tries to retroactively make Deangelo into a more concrete character by turning his ever-changing personality into a management strategy, it doesn't matter if the character isn't entertaining and if the situations he creates are dull. And while "Training Day" was at least able to lean on Michael's continued presence and the beginnings of his goodbye to Scranton, there is no such resonance here: Instead, it's just watching to see how an unfunny, poorly drawn character temporarily influences characters that we like but who lack any sense of direction.
That the episode ends with "What now?" is fitting given that we have no real way of answering that question, and this uncertainty is not in the show's best interest. Sure, you might argue that sheer curiosity is the only thing keeping some people watching after Carell's exit, but that will only sustain the show for so long (and perhaps only for thirty minutes). The show spent so much time building towards Michael's exit that they had nothing else to rely on in terms of recurring storylines, and the fact that Deangelo scrambles his brain at episode's end renders this episode filler. For the show to justify the time spent with Deangelo, I expected them to really look at how his presence might affect the characters more substantially, really laying out a roadmap for where the season might be headed. However, Andy largely reverted back to the same character he was before last week's successful sales call (left outside of the inner circle, and then throwing away all scruples once he's invited in), and it doesn't feel as though Deangelo made much of an impact on any other characters. At this point, Jordan the attractive executive assistant may be his only legacy, and there's a good chance she'll have disappeared by the time next week rolls around.
When I was among those having issues with the character of Pierce on Community earlier this season, I argued that it was an issue where the function of the character's cruelty wasn't worth it if that cruelty wasn't particularly funny (which, for me, it wasn't). However, in this case, we have a character who both wasn't funny and lacked any function or purpose. The existence of Deangelo was convenient in Michael's goodbye episodes, but it never felt essential, and it certainly was never funny enough to be considered worthwhile. It was a waste of time, to put it plainly, and I would be very curious to know what the show's plan for Michael's exit was before Will Ferrell basically offered himself a role on the show. Was there a plan for a more subtle introduction of a new boss, perhaps leaving more time for the other character to rise to the occasion of Michael's absence? It's a counterfactual that we'll likely never know the answer to, but one I can't help but wonder about given the quality of this episode and Ferrell's arc in general.
To be fair to "The Inner Circle," the parts of the episode not involving Deangelo weren't terrible. I liked that we saw more of Ryan and Kelly than we usually get to see, and that Kelly got to take a more authoritative role for a change. Kelly's a character whose level of intelligence is always somewhat variable, especially when it comes to Ryan, but to see her shift away from her swooning over Ryan as he fakes being her supervisor was quite satisfying. Similarly, I thought Dwight's refusal to engage with Deangelo was the one (welcome) bit of continuity from Michael's exit, and Rainn Wilson (who is now the top-billed actor on the show) is at his best when he is allowed to play Dwight as someone with a purpose. He wasn't just being difficult with Deangelo because he's Dwight, he was doing it because of both a continued loyalty to Michael and because that's just who Dwight is. It was a subtle purpose, perhaps, but it helps keep the character grounded (in stark contrast to Deangelo, who never had that grounding and suffered because of it).
However, a few clever one-liners are not enough to sustain an episode that has such a substantial burden. Here is the episode that is supposed to convince skeptical viewers that the show can live on without Michael Scott, the episode that the decision to go on without Carell was not purely motivated by the dire state of NBC. Here was their chance to prove once and for all that the creative drive behind the series was not contingent on Michael Scott, and instead they spent the entire episode giving free rein to a character who becomes an invalid at episode's end and who will likely (and hopefully) never be seen again. And even if you argue that the show's only burden is to be funny, I fail to see how "The Inner Circle" could be seen as meeting that burden.
While this show may be a sitcom, and there's often an expectation that the events of one episode won't mean anything a week later, I don't think this is an excuse for how meaningless this arc has been. If Deangelo had been funny, then maybe one last hurrah in "The Inner Circle" would have been enjoyable. Similarly, if Deangelo had had a purpose beyond the metatextual reunion of Carell and Ferrell, then perhaps he would have left behind a foundation for future storylines. The fact is that, just a week after the show emphasized the importance of character to its connection with its audience, The Office failed to deliver a character (or an episode) that was either funny or functional at a time when they needed both more than perhaps ever before.
Stray Observations:
- Am I the only person who thought that final scene of a mentally damaged Deangelo was tonally off for the show? Deangelo's fate as a whole, really, just feels like Ferrell decided how his own character should go out and nobody bothered to suggest that this is not a show where that kind of scene would be way off the mark. Just terrible.
- To go to the "corrupt Pam" narrative that came out of our discussion of last week's episode, we have her trying to push her good friend Carla to the top of the list for the Executive Assistant job — drunk with power, that one.
- Speaking of things Pam is drunk with or was likely drunk during, Pam's young adult book series — The Horse Flyer — sounds bloody awful. Of course, that was the point, but still - it needs saying.
- There was a brief moment where Jim wondered aloud if this was what the rest of his life would be like, a thread that I hope they pick up next week - here, though, it was just a pivot into the Horse Flyer joke.
- "Once you've seen sausage being made, all you want to do is make sausage, because it's so much fun."
- "Your boy, Kevin Malone, is in the inner circle…which doesn't exist." [Loved Kevin's smile after this one.]
- "What could he possibly stand to gain from a real juggling routine?"
- "I wrote my own companion piece to the Vagina Monologues called the Penis Apologies."
- "I will see you at your place around 2am."
- "I will say what I need to say and soon I will say it in Chinese."
- "If I wanted to see a pissing contest, I'd lock Mose in the chicken coop."


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Next big opportunity: Bond bubble burstingDecember 12, 2012: 4:31 PM ET
It's going to be tough to call, but three of the world's biggest investors agree that the next big money-making opportunity will be when interest rates rise from their historic lows and the bond bubble bursts.
"The greatest fortune made in the next five years is probably going to be made by some group or individual who figures out when the interest rate market will turn," said billionaire David Rubenstein, co-founder of private equity firm Carlyle Group.
But the hard part is timing that turn. "I don't know what will burst the interest rate bubble," he said during a conference Wednesday hosted by The New York Times' Dealbook.
Related: Carlyle's Rubenstein: Where we're not investing
While Rubenstein didn't dare forecast when interest rate will begin to rise, fellow panelist Ray Dalio, founder of Bridgewater Associates, gave it a shot.
Warning that "he who lives by the crystal ball is destined to eat ground glass," Dalio predicted that interest rates could begin to turn toward the end of 2013.
The Federal Reserve, which has had policies in place to keep interest rates low since late 2008, said Wednesday that it will begin to reverse its easing policies when the job market improves substantially, with the unemployment rate falling to 6.5%, or when inflation exceeds 2.5% a year.
While it's not imminent, Dalio said that biggest opportunity next year will come from shorting bond markets around the world.>
Dalio also said there's a place for gold in the portfolio, and predicted that stocks and emerging market currencies will deliver stronger performances than bonds.
Meanwhile, Stephen Schwarzman, the founder and chief executive of private equity firm Blackstone Group, said he would move out of junk bonds, which come with fixed interest rates, into debt that offers floating rates, interest rates that would rise along with the market, including debt from highly leveraged banks.


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[Cosmic Sans via DESIGNTAXI]


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Punjabi language
|ਪੰਜਾਬੀ پنجابی
'Punjabi' written in Shahmukhi (top) and Gurmukhi (bottom) scripts
|Native to
|Punjab region
Native speakers
|Eastern Punjabi: 34 million (2011)[1]
Western Punjabi: 93 million (2015)[2]
Standard forms
Perso-Arabic (Shahmukhi)
Punjabi Braille
Laṇḍā (historical)
|Official status
Official language in
| Pakistan (Punjab)[3]
India (Punjab, Haryana, Chandigarh, Delhi, Himachal Pradesh)
|Language codes
pan – Eastern Punjabi
pnb – Western Punjabi
panj1256 Punjabi[4]
Areas of the Indian Subcontinent where Punjabi is natively spoken
|Punjabi edition of Wikipedia, the free encyclopedia
|Western Punjabi edition of Wikipedia, the free encyclopedia
Punjabi is an Indo-Aryan language. It is the first language of about 130 million people, and is the 10th most spoken language in the world. Most of the people who speak this language live in the Punjab region of Pakistan and India. It is also widely spoken in Haryana, India Himachal Pradesh, India and Delhi, India. It is spoken by the majority of the population of Pakistan.[5]
Punjabi developed from the ancient language of Sanskrit just like many other modern Indo-Aryan languages such as Hindi, Bengali, Urdu and Marathi. Punjabi is unusual among this group for being a tonal language.[6][7][8][9]
Punjabi is written in two different scripts, called Gurmukhī and Shahmukhī. Punjabi is the main language spoken by the Sikhs.[10] Most parts of the Guru Granth Sahib use the Punjabi language written in Gurmukhī, though Punjabi is not the only language used in Sikh scriptures. The Janamsakhis, stories on the life and legend of Guru Nanak (1469–1539), are early examples of Punjabi literature.
Punjabi has many dialects. The dialects are similar enough to each other that speakers can understand most of the dialects that are related to theirs. In India, the main dialects of Punjabi are: Majhi, Doabi, Malwi and Pwadhi. In Pakistan, the main dialects are Majhi, "Shahpuri", "Jhangvi", "Dhanni", Pothohari and Hindko.[11]
Majhi is Punjabi's standard dialect because it forms the standard for writing in Punjabi. It is spoken in the centre of Punjab, including the districts of Lahore, Sheikhupura, Kasur, Okara, Nankana Sahib, Faisalabad, Gujranwala, Sialkot, Narowal, Gujrat, Pakpattan, Hafizabad and Mandi Bahauddin. In India it is spoken in Amritsar, Tarn Taran Sahib and Gurdaspur districts.
Other dialects of Punjabi include Pahari, Rachnavi, Chenavari, Chhachi, Jandali, Ghebi. The Saraiki, spoken in southern Punjab, and Dogri, spoken in Kashmir, are closely related to Punjabi. The relation of several dialects to languages other than Punjabi creates problems in assigning them to one or another "language".[12][13][14]
Over 93% of people who speak Punjabi as their first language live in Pakistan and India. It is the most widely spoken native language in Pakistan. It is spoken as a first language by over 44% of Pakistanis. There were 76 million Punjabi speakers in Pakistan in 2008.[15] In India, Punjabi is spoken as a native language by 3% of the population. This was about 33 million in 2011.[16] It is the official language of the Indian states of Punjab and Haryana.
Punjabi is also spoken as a minority language in several other countries where large numbers of Punjabis have emigrated.In the United Kingdom, it is the second-most-commonly used language.[17] In Canada, it is the fourth-most-spoken language.[18] There were 1.3 million Punjabi speakers in the UK in 2000,[17] and 368,000 in Canada in 2006.[19]
Writing system
There are three ways to write Punjabi: Gurmukhī, Shahmukhī, and Devanāgarī. In the Punjab province of Pakistan, the script that is most used is Shahmukhī. The Majhi dialect is the written standard for Punjabi in both parts of Punjab.
- ↑ "Punjabi, Eastern" . Ethnologue. Ethnologue. Archived from the original on 12 July 2017. Retrieved 13 August 2017.
- ↑ "Punjabi, Western" . Ethnologue. Ethnologue. Archived from the original on 12 July 2017. Retrieved 13 August 2017.
- ↑ "Pakistan Census" . Census.gov.pk. Archived from the original on 12 September 2011. Retrieved 4 January 2014.
- ↑ Hammarström, Harald; Forkel, Robert; Haspelmath, Martin, eds. (2017). "Punjabi" . Glottolog 3.0. Jena, Germany: Max Planck Institute for the Science of Human History.
- ↑ Pakistan Census
- ↑ Barbara Lust, James Gair. Lexical Anaphors and Pronouns in Selected South Asian Languages. Page 637. Walter de Gruyter, 1999. ISBN 978-3-11-014388-1.
- ↑ "Punjabi language and the Gurmukhi and Shahmuhi scripts and pronunciation" . Omniglot.com. Retrieved 2012-08-03.
- ↑ Phonemic Inventory of Punjabi
- ↑ Geeti Sen. Crossing Boundaries. Orient Blackswan, 1997. ISBN 978-81-250-1341-9. Page 132. Quote: "Possibly, Punjabi is the only major South Asian language that has this kind of tonal character. There does seem to have been some speculation among scholars about the possible origin of Punjabi's tone-language character but without any final and convincing answer..."
- ↑ Melvin Ember, Carol R. Ember, Ian A. Skoggard, ed. (2005). Encyclopedia of Diasporas: Immigrant and Refugee Cultures Around the World. Springer. p. 1077. ISBN 978-0-306-48321-9.CS1 maint: multiple names: editors list (link)
- ↑ Grierson, George A. 1904–1928. Grierson's Linguistic Survey of India . Calcutta.
- ↑ Masica, Colin (1991) The Indo-Aryan languages. Cambridge Univ. Press. p 25.
- ↑ Burling, Robbins. 1970. Man's many voices. New York: Holt, Rinehart and Winston.
- ↑ Shackle, C. 1972. Punjabi. London: English Universities Press. p 240.
- ↑ Pakistan 1998 census – Population by mother tongue
- ↑ Indian Census
- ↑ 17.0 17.1 McDonnell, John (7 March 2000). "Punjabi Community" . Parliamentary Business: Commons Debates. UK Parliament. p. Column 142WH. Retrieved 15 July 2012.
- ↑ "Punjabi is 4th most spoken language in Canada" . The Times of India. 14 February 2008.
- ↑ Population by mother tongue in Canada
More reading
|Punjabi edition of Wikipedia, the free encyclopedia
Punjabi phrasebook travel guide from Wikivoyage
- Bhatia, Tej (1993 and 2010) Punjabi: a cognitive-descriptive grammar. London: Routledge. Series: Descriptive grammars.
- Singh, Maya (1895) The Panjabi dictionary . Lahore: Munshi Gulab Singh & Sons.
- Ethnologue: Languages of India and Pakistan
Categories: Language articles with speaker number undated | Languages with ISO 639-2 code | Languages with ISO 639-1 code | Punjabi language | Languages of India | Languages of Punjab (Pakistan)
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Frequent Links
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or "dwarf" stars.[1][2]
After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.
The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, while main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.
In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, while stars with up to ten solar masses pass through a red giant stage.[3] More massive stars can explode as a supernova,[4] or collapse directly into a black hole.
In the early part of the 20th century, information about the types and distances of stars became more readily available. The spectra of stars were shown to have distinctive features, which allowed them to be categorized. Annie Jump Cannon and Edward C. Pickering at Harvard College Observatory developed a method of categorization that became known as the Harvard Classification Scheme, published in the Harvard Annals in 1901.[6]
In Potsdam in 1906, the Danish astronomer Ejnar Hertzsprung noticed that the reddest stars—classified as K and M in the Harvard scheme—could be divided into two distinct groups. These stars are either much brighter than the Sun, or much fainter. To distinguish these groups, he called them "giant" and "dwarf" stars. The following year he began studying star clusters; large groupings of stars that are co-located at approximately the same distance. He published the first plots of color versus luminosity for these stars. These plots showed a prominent and continuous sequence of stars, which he named the Main Sequence.[7]
At Princeton University, Henry Norris Russell was following a similar course of research. He was studying the relationship between the spectral classification of stars and their actual brightness as corrected for distance—their absolute magnitude. For this purpose he used a set of stars that had reliable parallaxes and many of which had been categorized at Harvard. When he plotted the spectral types of these stars against their absolute magnitude, he found that dwarf stars followed a distinct relationship. This allowed the real brightness of a dwarf star to be predicted with reasonable accuracy.[8]
Of the red stars observed by Hertzsprung, the dwarf stars also followed the spectra-luminosity relationship discovered by Russell. However, the giant stars are much brighter than dwarfs and so, do not follow the same relationship. Russell proposed that the "giant stars must have low density or great surface-brightness, and the reverse is true of dwarf stars". The same curve also showed that there were very few faint white stars.[8]
In 1933, Bengt Strömgren introduced the term Hertzsprung–Russell diagram to denote a luminosity-spectral class diagram.[9] This name reflected the parallel development of this technique by both Hertzsprung and Russell earlier in the century.[7]
As evolutionary models of stars were developed during the 1930s, it was shown that, for stars of a uniform chemical composition, a relationship exists between a star's mass and its luminosity and radius. That is, for a given mass and composition, there is a unique solution for determining the star's radius and luminosity. This became known as the Vogt-Russell theorem; named after Heinrich Vogt and Henry Norris Russell. By this theorem, once a star's chemical composition and its position on the main sequence is known, so too is the star's mass and radius. (However, it was subsequently discovered that the theorem breaks down somewhat for stars of non-uniform composition.)[10]
A refined scheme for stellar classification was published in 1943 by W. W. Morgan and P. C. Keenan.[11] The MK classification assigned each star a spectral type—based on the Harvard classification—and a luminosity class. The Harvard classification had been developed by assigning a different letter to each star based on the strength of the hydrogen spectral line, before the relationship between spectra and temperature was known. When ordered by temperature and when duplicate classes were removed, the spectral types of stars followed, in order of decreasing temperature with colors ranging from blue to red, the sequence O, B, A, F, G, K and M. (A popular mnemonic for memorizing this sequence of stellar classes is "Oh Be A Fine Girl/Guy, Kiss Me".) The luminosity class ranged from I to V, in order of decreasing luminosity. Stars of luminosity class V belonged to the main sequence.[12]
When a protostar is formed from the collapse of a giant molecular cloud of gas and dust in the local interstellar medium, the initial composition is homogeneous throughout, consisting of about 70% hydrogen, 28% helium and trace amounts of other elements, by mass.[13] The initial mass of the star depends on the local conditions within the cloud. (The mass distribution of newly formed stars is described empirically by the initial mass function.)[14] During the initial collapse, this pre-main-sequence star generates energy through gravitational contraction. Upon reaching a suitable density, energy generation is begun at the core using an exothermic nuclear fusion process that converts hydrogen into helium.[12]
Once nuclear fusion of hydrogen becomes the dominant energy production process and the excess energy gained from gravitational contraction has been lost,[15] the star lies along a curve on the Hertzsprung–Russell diagram (or HR diagram) called the standard main sequence. Astronomers will sometimes refer to this stage as "zero age main sequence", or ZAMS.[16] The ZAMS curve can be calculated using computer models of stellar properties at the point when stars begin hydrogen fusion. From this point, the brightness and surface temperature of stars typically increase with age.[17]
A star remains near its initial position on the main sequence until a significant amount of hydrogen in the core has been consumed, then begins to evolve into a more luminous star. (On the HR diagram, the evolving star moves up and to the right of the main sequence.) Thus the main sequence represents the primary hydrogen-burning stage of a star's lifetime.[12]
The majority of stars on a typical HR diagram lie along the main-sequence curve. This line is pronounced because both the spectral type and the luminosity depend only on a star's mass, at least to zeroth-order approximation, as long as it is fusing hydrogen at its core—and that is what almost all stars spend most of their "active" lives doing.[18]
The temperature of a star determines its spectral type via its effect on the physical properties of plasma in its photosphere. A star's energy emission as a function of wavelength is influenced by both its temperature and composition. A key indicator of this energy distribution is given by the color index, B − V, which measures the star's magnitude in blue (B) and green-yellow (V) light by means of filters.[note 1] This difference in magnitude provides a measure of a star's temperature.
Dwarf terminology
Main-sequence stars are called dwarf stars, but this terminology is partly historical and can be somewhat confusing. For the cooler stars, dwarfs such as red dwarfs, orange dwarfs, and yellow dwarfs are indeed much smaller and dimmer than other stars of those colors. However, for hotter blue and white stars, the size and brightness difference between so-called dwarf stars that are on the main sequence and the so-called giant stars that are not becomes smaller; for the hottest stars it is not directly observable. For those stars the terms dwarf and giant refer to differences in spectral lines which indicate if a star is on the main sequence or off it. Nevertheless, very hot main-sequence stars are still sometimes called dwarfs, even though they have roughly the same size and brightness as the "giant" stars of that temperature.[19]
The common use of dwarf to mean main sequence is confusing in another way, because there are dwarf stars which are not main-sequence stars. For example, a white dwarf is the dead core of a star that is left after the star has shed its outer layers, that is much smaller than a main-sequence star-—roughly the size of the Earth. These represent the final evolutionary stage of many main-sequence stars.[20]
By treating the star as an idealized energy radiator known as a black body, the luminosity L and radius R can be related to the effective temperature <math>T_{\rm eff}</math> by the Stefan–Boltzmann law:
- L = 4πσR2Teff4
where σ is the Stefan–Boltzmann constant. As the position of a star on the HR diagram shows its approximate luminosity, this relation can be used to estimate its radius.[21]
The mass, radius and luminosity of a star are closely interlinked, and their respective values can be approximated by three relations. First is the Stefan–Boltzmann law, which relates the luminosity L, the radius R and the surface temperature Teff. Second is the mass–luminosity relation, which relates the luminosity L and the mass M. Finally, the relationship between M and R is close to linear. The ratio of M to R increases by a factor of only three over 2.5 orders of magnitude of M. This relation is roughly proportional to the star's inner temperature TI, and its extremely slow increase reflects the fact that the rate of energy generation in the core strongly depends on this temperature, while it has to fit the mass–luminosity relation. Thus, a too high or too low temperature will result in stellar instability.
A better approximation is to take <math>\epsilon = L / M</math>, the energy generation rate per unit mass, as ε is proportional to TI15, where TI is the core temperature. This is suitable for stars at least as massive as the Sun, exhibiting the CNO cycle, and gives the better fit R ∝ M0.78.[22]
Sample parameters
The table below shows typical values for stars along the main sequence. The values of luminosity (L), radius (R) and mass (M) are relative to the Sun—a dwarf star with a spectral classification of G2 V. The actual values for a star may vary by as much as 20–30% from the values listed below.[23]
Table of main-sequence stellar parameters[24] Stellar
Radius Mass Luminosity Temperature Examples[25] R/R☉ M/M☉ L/L☉ K O6 18 40 500,000 38,000 Theta1 Orionis C B0 7.4 18 20,000 30,000 Phi1 Orionis B5 3.8 6.5 800 16,400 Pi Andromedae A A0 2.5 3.2 80 10,800 Alpha Coronae Borealis A A5 1.7 2.1 20 8,620 Beta Pictoris F0 1.3 1.7 6 7,240 Gamma Virginis F5 1.2 1.3 2.5 6,540 Eta Arietis G0 1.05 1.10 1.26 5,920 Beta Comae Berenices G2 1.00 1.00 1.00 5,780 Sun[note 2] G5 0.93 0.93 0.79 5,610 Alpha Mensae K0 0.85 0.78 0.40 5,240 70 Ophiuchi A K5 0.74 0.69 0.16 4,410 61 Cygni A[26] M0 0.63 0.47 0.063 3,920 Gliese 185[27] M5 0.32 0.21 0.0079 3,120 EZ Aquarii A M8 0.13 0.10 0.0008 2,660 Van Biesbroeck's star[28]
Energy generation
All main-sequence stars have a core region where energy is generated by nuclear fusion. The temperature and density of this core are at the levels necessary to sustain the energy production that will support the remainder of the star. A reduction of energy production would cause the overlaying mass to compress the core, resulting in an increase in the fusion rate because of higher temperature and pressure. Likewise an increase in energy production would cause the star to expand, lowering the pressure at the core. Thus the star forms a self-regulating system in hydrostatic equilibrium that is stable over the course of its main sequence lifetime.[29]
Main-sequence stars employ two types of hydrogen fusion processes, and the rate of energy generation from each type depends on the temperature in the core region. Astronomers divide the main sequence into upper and lower parts, based on which of the two is the dominant fusion process. In the lower main sequence, energy is primarily generated as the result of the proton-proton chain, which directly fuses hydrogen together in a series of stages to produce helium.[30] Stars in the upper main sequence have sufficiently high core temperatures to efficiently use the CNO cycle. (See the chart.) This process uses atoms of carbon, nitrogen and oxygen as intermediaries in the process of fusing hydrogen into helium.
At a stellar core temperature of 18 Million Kelvin, the PP process and CNO cycle are equally efficient, and each type generates half of the star's net luminosity. As this is the core temperature of a star with about 1.5 M☉, the upper main sequence consists of stars above this mass. Thus, roughly speaking, stars of spectral class F or cooler belong to the lower main sequence, while class A stars or hotter are upper main-sequence stars.[17] The transition in primary energy production from one form to the other spans a range difference of less than a single solar mass. In the Sun, a one solar mass star, only 1.5% of the energy is generated by the CNO cycle.[31] By contrast, stars with 1.8 M☉ or above generate almost their entire energy output through the CNO cycle.[32]
The observed upper limit for a main-sequence star is 120–200 M☉.[33] The theoretical explanation for this limit is that stars above this mass can not radiate energy fast enough to remain stable, so any additional mass will be ejected in a series of pulsations until the star reaches a stable limit.[34] The lower limit for sustained proton–proton nuclear fusion is about 0.08 M☉ or 80 times the mass of Jupiter.[30] Below this threshold are sub-stellar objects that can not sustain hydrogen fusion, known as brown dwarfs.[35]
Because there is a temperature difference between the core and the surface, or photosphere, energy is transported outward. The two modes for transporting this energy are radiation and convection. A radiation zone, where energy is transported by radiation, is stable against convection and there is very little mixing of the plasma. By contrast, in a convection zone the energy is transported by bulk movement of plasma, with hotter material rising and cooler material descending. Convection is a more efficient mode for carrying energy than radiation, but it will only occur under conditions that create a steep temperature gradient.[29][36]
In massive stars (above 10 M☉)[37] the rate of energy generation by the CNO cycle is very sensitive to temperature, so the fusion is highly concentrated at the core. Consequently, there is a high temperature gradient in the core region, which results in a convection zone for more efficient energy transport.[30] This mixing of material around the core removes the helium ash from the hydrogen-burning region, allowing more of the hydrogen in the star to be consumed during the main-sequence lifetime. The outer regions of a massive star transport energy by radiation, with little or no convection.[29]
Intermediate mass stars such as Sirius may transport energy primarily by radiation, with a small core convection region.[38] Medium-sized, low mass stars like the Sun have a core region that is stable against convection, with a convection zone near the surface that mixes the outer layers. This results in a steady buildup of a helium-rich core, surrounded by a hydrogen-rich outer region. By contrast, cool, very low-mass stars (below 0.4 M☉) are convective throughout.[14] Thus the helium produced at the core is distributed across the star, producing a relatively uniform atmosphere and a proportionately longer main sequence lifespan.[29]
Luminosity-color variation
As non-fusing helium ash accumulates in the core of a main-sequence star, the reduction in the abundance of hydrogen per unit mass results in a gradual lowering of the fusion rate within that mass. Since it is the outflow of fusion-supplied energy that supports the higher layers of the star, the core is compressed, producing higher temperatures and pressures. Both factors increase the rate of fusion thus moving the equilibrium towards a smaller, denser, hotter core producing more energy whose increased outflow pushes the higher layers further out. Thus there is a steady increase in the luminosity and radius of the star over time.[17] For example, the luminosity of the early Sun was only about 70% of its current value.[39] As a star ages this luminosity increase changes its position on the HR diagram. This effect results in a broadening of the main sequence band because stars are observed at random stages in their lifetime. That is, the main sequence band develops a thickness on the HR diagram; it is not simply a narrow line.[40]
Other factors that broaden the main sequence band on the HR diagram include uncertainty in the distance to stars and the presence of unresolved binary stars that can alter the observed stellar parameters. However, even perfect observation would show a fuzzy main sequence because mass is not the only parameter that affects a star's color and luminosity. Variations in chemical composition caused by the initial abundances, the star's evolutionary status,[41] interaction with a close companion,[42] rapid rotation,[43] or a magnetic field can all slightly change a main-sequence star's HR diagram position, to name just a few factors. As an example, there are metal-poor stars (with a very low abundance of elements with higher atomic numbers than helium) that lie just below the main sequence and are known as subdwarfs. These stars are fusing hydrogen in their cores and so they mark the lower edge of main sequence fuzziness caused by variance in chemical composition.[44]
A nearly vertical region of the HR diagram, known as the instability strip, is occupied by pulsating variable stars known as Cepheid variables. These stars vary in magnitude at regular intervals, giving them a pulsating appearance. The strip intersects the upper part of the main sequence in the region of class A and F stars, which are between one and two solar masses. Pulsating stars in this part of the instability strip that intersects the upper part of the main sequence are called Delta Scuti variables. Main-sequence stars in this region experience only small changes in magnitude and so this variation is difficult to detect.[45] Other classes of unstable main-sequence stars, like Beta Cephei variables, are unrelated to this instability strip.
The total amount of energy that a star can generate through nuclear fusion of hydrogen is limited by the amount of hydrogen fuel that can be consumed at the core. For a star in equilibrium, the energy generated at the core must be at least equal to the energy radiated at the surface. Since the luminosity gives the amount of energy radiated per unit time, the total life span can be estimated, to first approximation, as the total energy produced divided by the star's luminosity.[46]
For a star with at least 0.5 M☉, once the hydrogen supply in its core is exhausted and it expands to become a red giant, it can start to fuse helium atoms to form carbon. The energy output of the helium fusion process per unit mass is only about a tenth the energy output of the hydrogen process, and the luminosity of the star increases.[47] This results in a much shorter length of time in this stage compared to the main sequence lifetime. (For example, the Sun is predicted to spend 130 million years burning helium, compared to about 12 billion years burning hydrogen.)[48] Thus, about 90% of the observed stars above 0.5 M☉ will be on the main sequence.[49] On average, main-sequence stars are known to follow an empirical mass-luminosity relationship.[50] The luminosity (L) of the star is roughly proportional to the total mass (M) as the following power law:
- <math>\begin{smallmatrix}L\ \propto\ M^{3.5}\end{smallmatrix}</math>
This relationship applies to main-sequence stars in the range 0.1–50 M☉.[51]
The amount of fuel available for nuclear fusion is proportional to the mass of the star. Thus, the lifetime of a star on the main sequence can be estimated by comparing it to solar evolutionary models. The Sun has been a main-sequence star for about 4.5 billion years and it will become a red giant in 6.5 billion years,[52] for a total main sequence lifetime of roughly 1010 years. Hence:[53]
- <math>\begin{smallmatrix} \tau_{\rm MS}\ \approx \ 10^{10} \text{years} \cdot \left[ \frac{M}{M_{\bigodot}} \right] \cdot \left[ \frac{L_{\bigodot}}{L} \right]\ =\ 10^{10} \text{years} \cdot \left[ \frac{M}{M_{\bigodot}} \right]^{-2.5} \end{smallmatrix}</math>
where M and L are the mass and luminosity of the star, respectively, <math>\begin{smallmatrix}M_{\bigodot}\end{smallmatrix}</math> is a solar mass, <math>\begin{smallmatrix}L_{\bigodot}\end{smallmatrix}</math> is the solar luminosity and <math>\tau_{\rm MS}</math> is the star's estimated main sequence lifetime.
Although more massive stars have more fuel to burn and might be expected to last longer, they also must radiate a proportionately greater amount with increased mass. Thus, the most massive stars may remain on the main sequence for only a few million years, while stars with less than a tenth of a solar mass may last for over a trillion years.[54]
The exact mass-luminosity relationship depends on how efficiently energy can be transported from the core to the surface. A higher opacity has an insulating effect that retains more energy at the core, so the star does not need to produce as much energy to remain in hydrostatic equilibrium. By contrast, a lower opacity means energy escapes more rapidly and the star must burn more fuel to remain in equilibrium.[55] Note, however, that a sufficiently high opacity can result in energy transport via convection, which changes the conditions needed to remain in equilibrium.[17]
In high-mass main-sequence stars, the opacity is dominated by electron scattering, which is nearly constant with increasing temperature. Thus the luminosity only increases as the cube of the star's mass.[47] For stars below 10 M☉, the opacity becomes dependent on temperature, resulting in the luminosity varying approximately as the fourth power of the star's mass.[51] For very low mass stars, molecules in the atmosphere also contribute to the opacity. Below about 0.5 M☉, the luminosity of the star varies as the mass to the power of 2.3, producing a flattening of the slope on a graph of mass versus luminosity. Even these refinements are only an approximation, however, and the mass-luminosity relation can vary depending on a star's composition.[14]
Evolutionary tracks
Once a main-sequence star consumes the hydrogen at its core, the loss of energy generation causes its gravitational collapse to resume. Stars with less than 0.23 M☉,[3] are predicted to directly become white dwarfs once energy generation by nuclear fusion of hydrogen at their core comes to a halt. In stars between this threshold and 10 M☉, the hydrogen surrounding the helium core reaches sufficient temperature and pressure to undergo fusion, forming a hydrogen-burning shell. In consequence of this change, the outer envelope of the star expands and decreases in temperature, turning it into a red giant. At this point the star is evolving off the main sequence and entering the giant branch. The path which the star now follows across the HR diagram, to the upper right of the main sequence, is called an evolutionary track.
The helium core of a red giant continues to collapse until it is entirely supported by electron degeneracy pressure—a quantum mechanical effect that restricts how closely matter can be compacted. For stars of more than about 0.5 M☉,[56] the core eventually reaches a temperature where it becomes hot enough to burn helium into carbon via the triple alpha process.[57][58] Stars with more than 5–7.5 M☉ can additionally fuse elements with higher atomic numbers.[59][60] For stars with ten or more solar masses, this process can lead to an increasingly dense core that finally collapses, ejecting the star's overlying layers in a Type II supernova explosion,[4] Type Ib supernova or Type Ic supernova.
When a cluster of stars is formed at about the same time, the life span of these stars will depend on their individual masses. The most massive stars will leave the main sequence first, followed steadily in sequence by stars of ever lower masses. Thus the stars will evolve in order of their position on the main sequence, proceeding from the most massive at the left toward the right of the HR diagram. The current position where stars in this cluster are leaving the main sequence is known as the turn-off point. By knowing the main sequence lifespan of stars at this point, it becomes possible to estimate the age of the cluster.[61]
See also
- ^ By measuring the difference between these values, this eliminates the need to correct the magnitudes for distance. However, see extinction.
- ^ The Sun is a typical type G2V star.
Suggested reading
Kippenhahn, Rudolf, 100 Billion Suns, Basic Books, New York, 1983.
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External links
- Charity, Mitchell (2001-06-04). "What color are the stars?". Vendian Systems. Retrieved 2008-11-26.
Unknown extension tag "indicator"


text:
The First fact is, you are lucky enough, as your birth number becomes (1+4) 5. Number 5 represents Mercury planet. These people are quite reserve in nature. A penchant inclination towards the field of arts is one of their prominent features. Therefore, most of these high fives are poet, artist and experts. These people win the trust of others In no time. Generosity towards strangers is also a special trait of these people. These people are unaffected by the company of bad or good peoples. Generally people born on 5th of the month are gentle in nature.
Lucky Day : 1, 5, 7, 14, 23,
Lucky Number : 18.104.22.168.9,32,41,50
Lucky Year : 2030, 2032, 2034, 2050, 2059, 2052
Ishtdev : Shri Ganesh, Shri Maha Lakshmi
Lucky color : Green, Violet, cream
The year ahead
Happy Birthday & welcome to special section of Webdunia . Here, We render the Astro update & shed light on the personality of the Birthday Boy/ Girl.
You will not carry forward the worries and sorrows of last year. This year brings you success at your each step. The year 2016 will be fruitful for the students, Employee businessman and housewives. If you are unmarried this year brings you a great chance to get hitched. A happy family life awaits you this year.
Celebs with birth number 5
Sanjay Gandhi
Subhas Chandra Bose
William Shakespeare
Abhishek Bachchan
Ramesh Sippy


text:
Royals rally to end slide behind Butler's hustle
Perez plates go-ahead run in two-out eighth-inning charge
KANSAS CITY -- How many times has Ned Yost seen a game turn on Billy Butler's speed? The Royals' manager had to laugh.
"Not many," Yost said, "but I'm glad it did today."
That's exactly what happened as Butler, who plods like a plow horse, twice hustled to beat potential third-out plays during the Royals' eighth-inning rally that pulled them past the Washington Nationals, 6-4, on Sunday at Kauffman Stadium. The victory ended the Royals' seven-game skid as well as the Nationals' five-game winning streak.
Nationals reliever Craig Stammen was entrusted with a 4-4 tie and got two outs in the eighth before walking Eric Hosmer. Up came Butler, who hit a sharp grounder that bounced off and away from first baseman Adam LaRoche.
"At first, I just kind of stood there and thought, 'I hit it hard again but it's right at him at first.' So I thought for sure I'm out," Butler said. "But then when I saw it ricochet off, I ran hard to the bag. The reason I thought I was out was I wasn't even out of the box yet when the ball got to him."
Meanwhile, Stammen moved belatedly to cover first base.
"I just froze," Stammen said. "When it bounced away, I was like, 'Go after the ball or go to the base?' Obviously, I needed to go to the base."
"That's what cost them," Butler said. "The pitcher is supposed to get over there. They'd have had me, I don't run very well. All I could do was run hard and I beat him."
LaRoche probably had time to get the slow-running Butler himself but wasn't real sure where the ball went.
"It was a cue shot from a righty. It's not something you can work on," LaRoche said. "Initially, I thought it kicked more towards the bag. I look back and it's headed toward the opposite direction. That was a big play. It would have got us out of the inning."
But Butler was safe. Now Yost had to wrestle with a decision of his own. Should he lift Butler for a pinch-runner?
"If we don't score, then Billy's bat is out of the lineup and we'll surely come back around," Yost said. "If it's the ninth, it's a no-brainer. But in the eighth, it's a bit more difficult situation."
So he let Butler run for himself. Stammen walked Mike Moustakas to load the bases and Salvador Perez hit a sharp bouncer to shortstop Ian Desmond. He bobbled the ball, then went for a forceout at third base -- where Butler was headed.
"My heart kind of sunk there for a minute," Yost confessed. "As soon as it was hit and I saw him going to third, I'm thinking maybe I should have pinch-ran for him there."
Never mind -- Butler beat Desmond's toss to third baseman Ryan Zimmerman.
"I saw it hit the ground on my second step," Butler said. "I knew that potentially his only play might be to third so I was digging. On a ball like that, you don't usually see a guy try to throw to third for a forceout. I didn't know he bobbled it, but when it hit the ground, I was getting after it as hard as I could."
Hosmer scored the go-ahead run and the crowd of 19,661 went bananas. Perez was credited with an RBI single on the tiebreaking play.
"I knew I hit it pretty good but as soon as I saw to the right side, I thought I had a chance," Perez said. "Billy did a good job of running the bases hard."
David Lough then singled sharply to right field and Butler chugged home with an insurance run. Moustakas was thrown out trying to score on the same play, but the Royals had a two-run lead.
Closer Greg Holland pitched past two Nationals singles in the ninth inning, and the Royals' skid was over.
"We haven't had any breaks go our way the last week and we had a few today," Holland said.
The Royals jumped on right-hander Dan Haren for four runs in the first inning. Alex Gordon led off with a home run and Perez followed Moustakas' single with a two-run blast. In between, Emilio Bonifacio walked and sped all the way from first base to score as Hosmer's single bounced away from Desmond.
"That's part of my game and when we're not scoring runs, we have to find a way somehow," Bonifacio said.
Royals starter Ervin Santana gave up a fourth-inning solo homer to Desmond but otherwise kept control of the Nationals -- until there were two out in the seventh. Denard Span belted a home run, Zimmerman doinked a single and Bryce Harper ripped a two-run homer to left field for a 4-4 tie.
Santana survived a wicked shot to his right hip off Span's bat in the third inning, staying in the game after some tense moments while he shook off the pain.
"He threw the ball really well," Yost said. "I hated that he ended up giving up the tying runs so he didn't get the benefit of getting the win."
Kelvin Herrera took over and got through 1 1/3 scoreless innings and was rewarded with the victory when Holland notched his 35th save.
The victory enabled the Royals to go one game above .500 at 65-64.
"It's huge. You can't compete until you can win more games than you lose," Yost pointed out.
Now that the streaky Royals have ended this seven-game skid, they're yearning to start another winning burst.
"Especially this late in the season, if we want to make a run at this thing, we have to win some in a row again," Butler said.
"It feels good to get back on track," Hosmer said. "We still have the same goals in mind. We're going to finish strong and continue to come out and play it out. We've seen crazier things happen."
Like Butler winning a game with his speed.


text:
Now that the new year is here, you might be feeling a little crazy trying to organize all of those resolutions in your head. I've always found that jotting down those thoughts helps with the process of putting goals into action. Fortunately, there are plenty of apps available in the Google Play Store that offer this sort of thing: a place for Android users to put down their streams of consciousness, store photos that haven't been archived, or leave a mental note.
Catch, Free
Catch is an easy-to-use, quick access note-taking app that allows you to make text notes, leave voice memos, create reminders, and then share those items with friends and colleagues who also have the app. There's also a nifty widget that allows quick access to all of these features. If you're using the app for secret business or personal affairs, you can protect your data with a 4-digit PIN number. Upgrading to Catch Pro lets you attach PDF and Office files to your notes, create checklists, and upload up to 50GB of content.
Springpad, Free
If you're more of a collector than a note taker, Springpad lets you clip and gather things you find around the Web and then fetches contextual information for those things. For instance, if you clip the name of a movie you're dying to see, Springpad will fetch the Rotten Tomatoes review and nearby showtimes in case you decide you want to go see it right then and there. When you're finished, you can even invite your friends to join in on that list of movies you've got going to add their own. The app also enables you to clip articles, snap a photo, scan bar codes, record a voice memo, or save places of interest.
OneNote, Free
PC users may be especially thrilled to learn that Microsoft has a OneNote application available for Android devices. The app works similarly to the desktop version, enabling users to write notes, store pictures, and make to-do lists. It syncs up with Microsoft SkyDrive so that you can sync the data up in the cloud and access it elsewhere. One caveat, however, is that OneNote Mobile only allows up to 500 different notes; it will then require an upgrade for unlimited use via an in-app purchase.
Evernote, Free
The ultimate fan favorite, Evernote has been the top tier note-taking application for all mobile devices since its inception. The app allows users to sync notes across different devices (including computers and tablets), create and edit text notes and to-dos, share files, search within those notebooks, and share them with friends and colleagues via Facebook and Twitter. Evernote offers a few other extra features, like the ability to clip Web content from your desktop browser, or you can use the Evernote Smart Notebook by Moleskine to sketch ideas and then scan them into the app with your mobile device. If you decide you want more functionality, Evernote also offers Evernote Premium, a subscription service that lets you lock your notes with a numeric passcode, take notebooks offline on your mobile device, and allow others to edit your stuff.


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Dual-action gravity feed airbrush for fine art, nail art, temporary tattoo, cake decorating, hobbies, etc.
Color Media: Watercolor Pigments, Inks and Dyes, Acrylic, Automotive Urethanes, Lacquers, Enamels (Not Included).
0.3mm needle nozzle, broad spray, double action trigger for easy and accurate spray.
Made of high quality material, durable to use.
Easy fluid refills and easy cleaning.
Cup Capacity: 7ml(cc)
Nozzle: 0.3mm
Feed Type: Gravity
Pressure: 15-60PSI
Material: Metal
Color: Red, Gold
Package Included:
1 x 0.3mm Airbrush Spray Tool
1 x Wrench
1 x Straw
1 x Air Inlet Interface