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Shakti Pipe And Sanitary Stores
Address: Shop No.2, Shreeji Palace, S V Road, Kandivli (West), Mumbai, Maharashtra,
Phone number: +91-22-28074337Post A Recommendation Bookmark this Business Claim this Business
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Friday, December 31, 2010
Wednesday, December 29, 2010
Heather Parisi - Crilù
This isn't a S.A.W. production. It's an italian act, a song related to a 1985 Tv Show and the hollywood-italian show girl, first dancer is Heather Parisi. You have to see it! There are wonderful dance routines.
Pubblicato da Paolo 0 commenti
Etichette: Heather Parisi
Monday, December 27, 2010
Body Language
Kylie Minogue - 'I Believe In You ' Behind the scenes news feature
Kylie Minogue in the making of Giving You Up
Kylie Minogue - 'WOW ' Making Of...
This wasn't a Stock, Aitken & Waterman production
Mel & Kim - Respectable (Wacaday)
Mel & Kim - FLM (Montreux, 1st performance)
Mel & Kim - F.L.M. (Pete Hammond Remix Edit)
Mel & Kim feature on The Top Ten of 1987
With Mike Stock and Pete Waterman talking about the famous duo they produced.
Pubblicato da Paolo 0 commenti
Etichette: Mel and Kim, Mike Stock, Pete Waterman
Sunday, December 26, 2010
Sabrina - Hot Girl. (ZDF)
This song was produced by the italian C.Cecchetto, it wasn't a Stock, Aitken & Waterman production, but they remixed it.
The original video:
Pubblicato da Paolo 0 commenti
Etichette: Sabrina
The London Boys on TV-AM (1989)
LONDON BOYS: "Freedom" (Good audio quality!)
London Boys - My Love
Saturday, December 25, 2010
Big Fun featuring CBBC presenters - Can't Shake The Feeling (December 1989)
Big Fun performing Can't Shake The Feeling. Also featuring CBBC presenters Andy Crane, Andy Peters, and Simon Parkin, a Stock, Aitken & Waterman production.
Pubblicato da Paolo 1 commenti
Etichette: Big Fun
Saturday, December 18, 2010
STEPS - Last Thing On My Mind
STEPS - Loves Got A Hold On My Heart
H&CLAIRE - Half A Heart - (The Brian Conley Show)
Pubblicato da Paolo 0 commenti
Etichette: H and Claire
H&CLAIRE - Beauty And The Beast - (Top Of The Pops)
Pubblicato da Paolo 0 commenti
Etichette: H and Claire
Kylie Minogue - All The Lovers (Cover)
Informations about the song "All The Lovers", here in Wikipedia.
- Jim Eliot – songwriting, production, piano, keyboards, bass and drum programming
- Mima Stilwell – songwriting, additional backing vocals
- Stuart Price – additional production, mixing
- Dave Emery – mixing assistant
Pat & Mick Use It Up Wear It Out - Top of the Pops April 1990
From Wikipedia:
Pat and Mick were a British vocal duo consisting of popular radio personalities Pat Sharp and Mick Brown. The royalties from their record sales were donated to Capital FM's 'Help A London Child' charity. All their singles were produced by Stock Aitken & Waterman.
The pair were often portrayed as unintelligent in media coverage, but this served to boost record sales, providing money for the charity in the process.
With their last single released in 1993, and Sharp no longer at Capital Radio, they have no immediate plans to collaborate on future charity singles.
As of February 2009, Brown is hosting the 'Drive Time' radio show on 107.8 Radio Jackie, while Sharp presents the same slot on Heart Cambridge.
- 1988: "Let's All Chant" / "On The Night" (UK #11, credited to 'Mick And Pat')
- 1989: "I Haven't Stopped Dancing Yet" (UK #9)
- 1990: "Use It Up and Wear It Out" (UK #22)
- 1990: "Ole Ole Ole" (released under the name L.A. Mood) (UK #78)
- 1991: "Gimme Some" (UK #53)
- 1991: "The Concrete Megamix"
- 1992: "Shake Your Groove Thing"
- 1993: "Hot Hot Hot" (UK #47)
- 1993: Don't Stop Dancin'
Pubblicato da Paolo 0 commenti
Etichette: Pat and Mick
Pat and Mick - I Haven't Stopped Dancing Yet
Pubblicato da Paolo 0 commenti
Etichette: Pat and Mick
Big Fun - Can't Shake That Feeling (Live in Norway)
Another Stock, Aitken & Waterman production:
Pubblicato da Paolo 0 commenti
Etichette: Big Fun
Kiss Like This - Faith in you
from YouTube:
"Found this track on an old compliation video i have, very PWL sounding - dont know much else about this group! Producers - Steve Jolley , Tony Swain, Jolley & Swain producers."
Pubblicato da Paolo 0 commenti
Etichette: Kiss Like This
Bananarama - I heard a rumour Live 1987
Another Stock, Aitken & Waterman production:
Kylie Minogue - I Believe In You (Orchestral Version)
Sunday, December 12, 2010
Bananarama - I Can't Help It (Live from Spain)
The original Bananarama group, live including Siobhan on a Spanish TV Show, singing a song produced by Stock, Aitken & Waterman.
Sunday, December 5, 2010
Kylie Minogue - Making of Never Too Late
A song produced by Stock, Aitken & Waterman, "Never Too Late"
Pubblicato da Paolo 1 commenti
Etichette: Kylie Minogue
Kylie Minogue - Making Of Colour your life ad
Bananarama Interview Voyage, Voyage Live Maison Folie, Lille 4/3/2008
Bananarama - The Alan Titchmarsh Show
Bananarama : Loose Women
THE SHEILAS - (I'm So) Happy, Happy (You're Mine)
The Sheilas, high resolution video. I liked very much this new Stock, Aitken & Waterman production. But the video is a little poor. It was a shame this song has not been successful.
Pubblicato da Paolo 0 commenti
Etichette: The Sheilas

subset: commoncrawl


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- Duration
3-4 hours.
- Group Size
Minimum of 8 hens.
- Availability
7 days a week.
- Seasonal
All year round.
- Dress Code
Swimwear, towel, sandals.
Please note...
Please Note: This page provides a general guide to our spa and buffet lunch in Benidorm. We work with multiple suppliers, so please be aware that specifics may vary. Feel free to ask your Destination Specialist at the time of booking if you have any questions about this.


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Rulan Allwine is an innkeeper in Market Sheran, a village in Andor.
He is a stout man.
When Rand al'Thor and Matrim Cauthon are making their way to Caemlyn, they stop at Rulan's inn. Rand and Mat are shocked at the prices he is charging, due to the hard times. Nevertheless, they stay at his inn for the night.[1]


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We promise that someone will get back to you to talk through your situation and explain how we can help. You can expect to hear back from us within two working hours and certainly no later than 10 am on the next working day.
Sorry, there are a few problems with the information you have entered. Please correct these before continuing.
Your submission has been received. We'll be in touch soon.
Breach of covenant claims are more usually taken by the landlord against the tenant and can include circumstances such as failure to pay the rent, sub-letting without permission, carrying out unauthorised alterations, failure to repair or maintain as required (dilapidations) or becoming insolvent.
A landlord may be equally guilty of breaching covenants if they fail to meet their obligations contained in the lease such as wrongly withholding or delaying consent for assignment, subletting or alterations, breach of 'quiet enjoyment' (the tenant's right to live in and use the rented property without unwarranted interference from the landlord) or a failure to insure the property.


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Details & Care
Vivid, variegated stripes pattern a slim crewneck sweater knit from a cozy cotton blend.
- Approx. length from shoulder: 26 1/2".
- Measurements taken from size Medium and may vary slighlty by size.
- Cotton/acrylic/polyamide; machine wash or dry clean.
- By Hugo Boss; imported.
- Men's Sportswear.
- Learn more about the Hugo Boss labels.
- Item #636320


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By: Nolan Haren and Dalton Rayman
Computer Programming
Software Engineer
Computer Programmer
A computer programmer writes programs, debugs, tests other software, programs the software and debugs them. It is ranked #5 in the Best Tech Jobs list and #13 in the 100 best jobs list. You need to be able to convert what needs to happen into a computer "language" such as C++ or Python. Many require a bachelor's degrees.
This is C++
Computer Programming
Computer programmers make a median salary of $74,280. The bottom 10% make an hourly pay of $20.60, the next 15% at $27.13 an hour 75% with $45.26 and the top 10% make $56.68 dollars an hour!
Software Engineer
A computer software engineer is an expert at computing, system designs, and maintaining software. Computer software engineers fall into two categories; computer applications and computer systems. A computer software engineer will work on a host of projects. These professionals are often extremely detailed. A software engineer constantly needs to keep up with his profession, as new programming languages and technologies emerge.
You typically need to be very good in math in order to acquire this job.
Software Engineer
Software Engineer's start with a $54,840 annual salary and that can grow anywhere from $132,080 or often times more. In DC alone, there are over 20+ offices that offer a 100,000+ annual salary.
Present Remotely
Send the link below via email or IMCopy
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Nolan Harenon 8 January 2014
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Listen to free music by Kochschützstuderamstad
Blip.fm is internet radio made social. It's easy to search for, play, and discover free music recommended by real people. Join today to create your own free station.
Artists Like Kochschützstuderamstad
Blip.fm DJs who play Kochschützstuderamstad
Friends: MerchantCircle | Charity Blossom | Website Load Testing


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The Faculty Center enables you to manage much of your on-campus life from one place, and is accessed through the myHumboldt portal. Powered by Oracle's PeopleSoft software, the Center is designed to enhance productivity by making it easy to access the data you need, which ultimately improves efficiency for all users.
In the Faculty Center, you can
A current browser is all that's needed to access the Faculty Center.
Mac users should use Firefox; Safari is not compatible with PeopleSoft applications.
Please note that the Faculty Center may be down for routine maintenance every Wednesday from 6:00pm-10:00pm. For more information, check the server maintenance schedule.
Access the Faculty Center online through myHumboldt.
Like any other online service at HSU, you'll need your HSU User Name and Password to log into the Faculty Center.
When you log into the Faculty Center, you'll see an overview of your current situation - just click on any link to drill down into that area for more information.
A number of PDFs are available on the main Faculty Center web page that will guide you through different aspects of the site. You can also request a Live Demo by clicking on the appropriate link on the right side of the Faculty Center web page.
The Faculty Center, like myHumboldt itself, is protected by a time-out period which logs you out of the application if you have not accessed it 45 minutes. You'll see a warning message before the system logs you out, at which point you can choose to stay logged in.
Think security when you log out of an application or myHumboldt and be sure to close your browser to fully quit or exit the application.
If you have ever taken classes at HSU, you'll find you also have a Student Center page.
The primary policy governing faculty use of campus administration software is the CSU Responsible Use Policy.


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Hellfire Blast, called Crimson Thunder Wave (雷紅波 raikōha) in the Japanese version, was introduced in Tekken 5 as part of Devil Jin's movelist. This move is similar to Devil's Inferno attack. Hellfire Blast is much faster than Inferno, and instead of shocking the opponent, it forcefully knocks the opponent to the ground. Notably, while Inferno had a range limit, Hellfire Blast will extent through the entire screen - but at farther distances there's a chance that the move will wander upwards before it reaches the opponent.
Hellfire Blast is a "high risk - high reward" move; though it can take a good chunk of health away, Devil Jin is at the mercy of the opponent if he misses. In most cases, the opponent has enough time to perform their strongest unblockable attack before Devil Jin regains control. The user can angle Hellfire Blast to the left or right by pressing Up or Down respectfully. Doing this slightly shortens the recovery time, but the user needs to be very close to the opponent to connect this way (or, on the off chance that the opponent side-steps in the same direction, it can be used at a distance).
Hellfire Blast can be avoided by simply crouching or sidestepping. For Jack models, they can recovers his health after attacked by this move.


text: Women itself is a beautiful word. But when you try to understand the nature of women then its a complete mystery. Its hard to understand what women are thinking at instant time. Women are not expressive like men. When it comes to Nepali women then its more complicated task. Here are some of the Nepali…[Continue reading]


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Public Sector and Government
San Francisco
San Francisco, CA - (USA) 275 Battery Street Suite 710 CA San Francisco , CA - 94111 Phone : 415-781-7171
Keefe Group- Since 1975, Keefe has services the correctional market exclusively and pioneered the evolution of products, packaging and technology services to fit the needs of facilities nationwide.
Commissary Representative
$14.00 Per Hour - part time: Must be available Wednesday & Thursday 1PM - 8PM
Deadline to Apply: January 11th 2017
**All applicants must fill out online application to be considered**
* Delivery of individually packaged orders to inmates at specified correctional facilities with the supervision of a correctional officer in a timely and efficient manner
* Obtain signature of inmate on 2 ply order receipt
* Note any and all discrepancies or damages on both copies of order receipt
* Must be a self-starter who can work well with people in a correctional facility in a professional, upbeat manner.
* Ability to work in a correctional environment.
* Ability to lift up to 50lbs.
* Must qualify for correctional facility security clearance.


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|Home > Bridge
♂ Bridge
What does Bridge mean?
Bridge [bridge] as a name for boys is of Old English derivation, and the name Bridge means "lives near the bridge; bridge-worker". Bridge is an alternate spelling of Bridger (Old English).
ASSOCIATED WITH old english, worker (occupational)
VariationsCREATIVE FORMS
(male) Birge, Burge, ..
(female) Bridde, Bridne, .. MIDDLE NAME PAIRINGS
Bridge Faris (B.F.), ..
How popular is Bridge?
Bridge is an uncommonly occurring first name for men but a very prominent last name for all people (#5383 out of 150436, Top 4%). (2000 U.S. DEMOGRAPHICS)
Which version is better?with its source form and related boy names. Bridger (#1019 LAST YEAR) is the only popular varying form of Bridge (NOT RANKED). Adoption of this relation of Bridge was common among parents 2 years ago (#907) and is almost as conventional today. (TOP 2000 NAMES, 2015)
Similar NamesRecommended names are Arledge, Arlidge, Bairre, Baldie, Bede, Beirne, Bid, Bidal, Bille, Bing, Bingo, Blade, Bligh, Blithe, Boid, Boine, Boyde, Bradan, Bradd, Braden▼, Bradey, Bradie, Bradin, Bradlea, Bradlee, Bradley▼, Bradly▼, Bradney, Bradon, Braidie, Braidin, Braydie, Brette, Briano, Briant, Brice, Bricio, Bricker, Bridgeley (see Bridgely), Bridgely, Brien, Brigg, Briggs▲, Brik, Briley, Brilie (see Briley), Brindly, Brinlee, Brinly, Brit, Briton, Britte (see Brett), Brizio, Brod, Broddy, Brodee, Broden, Broder, Brodey, Brodie, Brody, Bruce▼, Brucie, Brye, Bryse, Colridge (see Coleridge), Dodge, Elbridge, Gaige, Hodge, Lige▼, Ridge▲, Saige, Teige and Tige. These names tend to be more commonly used than Bridge.See names in meaning and etymology.


text:
Industry Insights
Brought to you by:
Tag, Poke and Follow
to your heart's content.
Guest Blog: Elma Glasgow, How Copywriting Can Give You Charisma
How copywriting can give you charisma!
Whether you're creating copy for print or digital, you must grab your customers' attention from the get-go. Use words that'll give them a wink, start a conversation and build rapport. When done with skill it could bring about a beautiful customer relationship!
Give your audience something that'll make their life better, easier, more fun, more luxurious, more…well, you get the picture. Give them something engaging. Something that'll win their hearts, as well as their minds!
How can you achieve such compelling copy? Well, it involves a combination of elements: structure, word-flow, punctuation, vocabulary, tone of voice and character. There's no doubt that good copywriting is a craft, but we're going to let you in on a few secrets that could make your marketing copy more magnetic.
- Put your customer first
Focussing on how your company was established when you actually want to promote your new heated-shiatsu-massaging car seats probably won't help you boost sales. As hinted above, to appeal to customers you need to put them first. When writing copy, think about what they want to know and how they want to feel. Inspired? Empowered? You also need to hold their attention by writing in a style that suits them. Your average luxury 4x4 driver is unlikely to respond to language more suited to two-door run-around owners!
- Give copy emotion
When used well just a few words can carry huge amounts of emotion. Images can help get the message across in a more immediate way. Take inspiration from charities, which rely on succinct copy to raise essential funds to carry out their vital work. They quite literally can't afford to get it wrong.
- Be confident
If you decide to hand over your project brief to a Cambridge copywriter you're opening up a wonderful opportunity to source fresh and exciting ideas that may not have occurred to you before. If the writer comes back with unexpected but engaging concepts, go with it. Be bold - break out of old habits and inject new energy into your marketing.
- Make it look effortless
Like soft clay, language needs to be played around with. It needs to be stretched and thrown around a bit before it takes shape. Replace the potter's wheel with a laptop and a dollop of imagination, and you have everything you need for some striking craftsmanship. By harnessing the power of punctuation (yes, apostrophes are important!), word-length and vocabulary, your copy can be moulded into something that flows nicely, making it easy for readers to absorb and instantly understand.
Also knowing how language works will help you smooth out inconsistent and rough copy that, when read, feels jarring. This is really important; your customers might not realise why the copy is hard work to read so they'll just to move on.
- Your promise – a building block of trust
If you run a business you already know never to promise what you can't deliver. Repeatedly disappointed customers lead to a loss in loyalty that could damage your reputation. A copywriter can write fantastic copy, but you need to be very clear on what you're offering. By developing an accurate project brief, the copy will reflect your product or service with authenticity and integrity.
Although this is just a small sample of techniques used to create charismatic copy (we can't give away all of the trade secrets!), we hope it comes in handy. If you'd like more advice, contact Red Ruby Copywriting today.
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text: Hytera launches intrinsically safe TETRA ATEX two-way radio 27 Apr 2016 12:43 PM Radio is certified to ATEX 'ia' standards, IP67 and MIL-STD-810 F/G and features other man down and lone worker functions, along with integrated GNSS positioning dataHytera introduced its first intrinsically safe TETRA handheld radio during the 360° conference in Dubai this week (26 April 2016). The PT790 Ex is tailored to the specific needs of users in sectors such as the oil and gas industries, mining or fire brigades.The radio achieved the highest grade 'ia' ATEX certification, enabling it to be used in environments which contain an explosive atmosphere of air and flammable gases, vapours or permanent mists (Zone 0).The new Hytera radio is also protected against dust and moisture according to protection class IP67 (30 minutes in a water depth of 1 meter) and meets the US military standard MIL-STD-810 F/G.To ensure the highest safety at work the PT790 Ex includes man down and lone worker functionalities. The integrated GNSS module collects positioning data via GPS, GLONASS and Beidou and can transmit the data to control centres or dispatchers with AVL for further analysis.In addition to the usual voice and data communications, the PT790 Ex provides many more features including encryption, programmable keys, etc. In addition, the handheld radio has an interface for extensions and accessories.The radio operates in the TETRA frequency ranges of 380– 30 MHz and 806–870 MHz. Itsdimensions are 141 mm high by 55 mm wide and 39 mm in depth and it weighs approximately 515 g (with 1800 mAh battery and antenna). It features a lithium-ion 1800 mAh battery, which will provide approximately 14 hours of operating life. Maximum audio power output is > 1.2 W.The radio features a 1.8 inch, 160 × 128 pixel, 65,536 colours LCD colour display and has an operating temperature range of - 30 °C bis + 60 °C in non-hazardous environments and - 20 °C bis + 55 °C in hazardous environments.The radio will be launched in Europe during the Critical Communications World 2016 conference and exhibition in Amsterdam, the Netherlands (31 May to 2 June 2016).Hytera already has two DMR (Digital Mobile Radio) ATEX hand portables in its portfolio – the PD795 Ex (with display screen) and PD715 Ex (without display screen).For more information on the TETRA PT790 Ex specifications go to:http://www.hytera-mobilfunk.com/tetra/radios/radio-details/details/pt790-ex/James Atkinson EditorLinkedIn |Google + |Email Leave a CommentPlease write code to prove you're humanThis article appeared in... Issue 41Log in to read all of Issue 41Free access to premium contentMore on... TetraMotorola launches all-in-one single site TETRA digital radio system Southern Tyrol TETRA network gets a workout at Biathlon World Cup Motorola scoops deal to provide 30,000 TETRA radios to German police More on... Critical CommunicationsFinland and Norway sign cross-border TETRA communication dealCC Europe 2017: Hytera showcasing new base station and handheld radioMore on... HyteraPennine delivers Hytera radio solution at Etihad Stadium in ManchesterHytera offer to acquire Sepura for £74m agreed by shareholdersLatest in PMRPennine delivers Hytera radio solution at Etihad Stadium in ManchesterTCCA pinpoints key focus areas for LTE-based critical communicationsTait appoints Andrew Gill as managing director of EMEA region


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The Solar Neutrino Problem
- Janice Ross
- 2 years ago
- Views:
1 The Solar Neutrino Problem Martin Lahrz University Umeå Abstract Since neutrinos are the only known particles being able to leave the core of the Sun directly, they were supposed to approve the Standard Solar Model. However, the number of detected neutrinos was only one third of the predicted number. [10] After theoretical computations and other experiments had corroborated our understanding of the Sun, the question of the missing neutrinos remained as the solar neutrino problem. Not until 2001 neutrino oscillations could explain this discrepancy [13] and gave in turn new insights about the neutrinos themselves. 1 Neutrinos and their classification 1.1 From Pauli to the Standard Model A two-body decay produces a discret energy spectrum since the conservation of energy and momentum ensure an unique solution. From the point of view in the early 1900s in the beta decay one electron is leaving the core which is changing its atomic number by one. However, in 1911 L. Meitner and O. Hahn verified a continuous spectrum of the electrons coming from the beta decay which was a contradiction. Additionally, the conservation of angular momentum was violated, too. In 1930 W. Pauli postulated a neutral particle with spin 1/2 which he called neutron [24]. Because of J. Chadwick s discovery of the todays neutron in 1932, E. Fermi, who worked out the theory about this particle, renamed it later to little neutron neutrino. In a three-body problem the energy spectrum of each participant would be continuous. According to Pauli the particle should be similar to light quanta but not travelling with the speed of light and the mass should be at the same magnitude as the electron mass. Simultaneously this particle could permeate matter as good as x-rays or even better since its cross section is very small. In fact, Pauli himself thought it would not be possible to see it for a long time. Indeed, this succeeded for the first time by C. Cowan and F. Reines [18] in So far, only the electron neutrino was known but J. Steinberger, M. Schwartz and L.M. Ledermann discovered with the muon neutrino a second generation in 1962 [19]. When M.L. Perl found the tauon in 1975 [25], physicists expected also a corresponding neutrino generation. In fact, it was verified at the DONUT experiment in 2000 [12] as the latest particle of the Standard Model being directly observed. 1.2 Properties Neutrinos are neutral charged elementary particles. As leptons they are fermions and have a spin of 1/2 which was already postulated by Pauli. As mentioned previously, three different flavors are known: electron neutrinos, muon neutrinos and tau neutrinos while each type has basically an antiparticle. It is for sure that there are exactly three generation with a mass less than 45.6 GeV [20]. Neutrinos interact through the weak force, primarily, and throught the gravitational force which is in most cases neglectable, however. Since they do not interact neither through the electromagnetic force nor through the strong force, their cross section is extremly small. On the one hand, this allows them to cross matter almost unaffected. Especially they are able to leave the Sun s core directly which make them to the only known information source about this region. On the other hand, it is very hard to verify these neutrinos here on Earth. The Standard Model of particle physics describes neutrinos as massless. According to the special theory of relativity this leads to the assumption that neutrinos must travel at the speed of light c. In fact, experiments with the MINOS detector measured their speed to (v c)/c = 5.1 ± (at 68% C.L.) [1] which at least means that it is very close to c. However, ob- 1
2 served neutrino oscillations, playing an important part in the solution of the solar neutrino problem, require a nonzero mass. 2 The solar neutrino problem 2.1 The Standard Solar Model The Standard Solar Model (SSM) desribes the structure and the thermodynamical properties of the Sun. According to the SSM the Sun generally consists of hydrogen plasma which is designed by the equilibrium of the gravitational force and the energy density. At the core temperatures of about K [21] and pressures of 150 g/cm 3[8] enable nuclear fusion where mainly a proton is transformed into a neutron. To verify the SSM different radiation or fluxes might be observed: photons in the sense of light, plasma namely the solar wind, and neutrinos. In contrast to all other particles including photons, neutrinos are coming right from the core and therefore can give particular insights into the Sun. Table 2.1: Neutrino production from the protonproton chain reaction (upper) and the CNO cycle (bottom) based on the SSM. The total solar flux at the Earth is cm 2 s 1. The majority of the solar neutrinos come from the pp chain (more than 91%); while the 7 Be, pep, and 8 B chains correspond to about 7%, 0.2%, and 0.008% of the total flux, respectively. The hep contribution is minuscule and mostly neglected. [9] This is table 7 of [6]. Reaction Label Flux cm 1 s 1 p + p 2 H + e + + ν e pp p + e + p 2 H + ν e pep He + p 4 He + e + + ν e hep Be + e 7 Li + ν e 7 Be B 8 Be + e + + ν e 8 B N 13 C + e + + ν e 13 N O 15 N + e + + ν e 15 O F 17 O + e + + ν e 17 F Neutrinos from the Sun Whenever a proton is converted in a neutron a quark has to change its flavor. The only interaction being responsible for this is the weak interaction and therefore the nuclear beta decay. Thus, each time a neutron is formed, an electron neutrino is produced, too. [9] p + X n + e + + ν e + X (1) These neutrinos have a continuous energy spectrum with a maximal energy depending on the reaction, see Tab. 2.1 as well as Fig However, the inverse beta decay of 7 Be produces a discret energy spectrum with lines at 0.9 MeV and 0.4 MeV. The flux of the 8 B neutrinos is of particular importance since it is Φ( 8 B) T 25, so highly sensitive. [5] This is only one example how neutrinos might give applicable information about a property of a system. 2.3 Homestake The first investigation of solar neutrions were made by R. Davis in the mid-1960 s. [4] The so-called Homestake experiment was based on the neutrino reaction on chlorine making an isotope of argon Figure 2.1: The solar neutrino spectra predicted by the SSM. Note, that the continuum neutrino fluxes at one astronomical unit are given in units of cm 2 s 1 MeV 1, while the line ones are given in cm 2 s 1. This is figure 2 of [7]. ν e + 37 Cl e + 37 Ar (2) 2
3 where the minimum energy of the neutrinos have to be MeV. This reaction is very rare and according to Fig. 2.1 a large percentage of incoming neutrinos just drop out. In fact, about one atom of argon was produced each week in a tank containing about 380 m 3 of the dry-cleaning fluid, perchlorethylene. [9] However, neutrinos coming from Earth were precluded easily since there are no sources connected with these energies. Already the first results from 1968 showed two aspects. First, argon atoms were produced, i.e. the experiment was working. But second, the number of measured events was only about a quarter of the expected number. Finally, the experiment ended in 1995 and led to the following result, which still was unsatisfying: [10] Φ Cl (Homestake) = 2.56 ± 0.16 ± 0.16 SNU, while the SSM predicted Φ Cl (SSM) = SNU. Note: A SNU (Solar Neutrino Unit) is the product of the solar neutrino fluxes, measured or calculated, and the calculated cross sections. Hence one SN U equals one capture per second and per target atoms. [9] In consideration of this result, either the Standard Solar Model or the Standard Model of particle physics had to be revised. On the one hand, other observation confirmed the SSM. On the other hand, a change of the neutrino flavor contradict the Standard Model of particle physics since neutrinos have no mass according to this model. In fact, neutrino oscillations were postulated in the case of a nonzero mass by B. Pontecorvo in 1957 [26]. 2.4 SAGE and GALLEX/GNO Since Homestake was only able to detect high energy neutrinos, two other experiments working with gallium were conceived. The Soviet-American Gallium Experiment (SAGE) was located in the Baksan laboratory in Russia, the Gallium Experiment (GALLEX) and later Gallium Neutrino Observatory (GNO) were an European project situated in Italy. The underlying reaction ν e + 71 Ga e + 71 Ge (3) is very similar to Eq. (2) but already sensitive for energies of at least MeV including pp, 7 Be, 8 B, and pep neutrinos. The expected flux was more than 15 times higher than with chlorine. Indeed, both independent experiments came to a similar results [9] Φ Cl (SAGA) = SNU Φ Cl (GALLAX/GNO) = 70.8 ± 4.5 ± 3.8 SNU but the flux predicted by the SSM [9] Φ Cl (SSM) = SNU was still about twice as large. 2.5 Kamiokande and SuperKamiokande In 1987 the Kamiokande experiment changed the reference method fundamentally using a water Čerenkov detector instead of a radiochemical one like the previous experiments did. The neutrino-electron scattering process 1 ν e + e ν e + e (4) accelerated the electrons to a velocity above the speed of light in water which cause characteristic Čerenkov radiation. This radiation can be evaluated by photomultiplier tubes in intensity and direction. The primal experiment was supposed to determine the direction of incoming neutrinos in general. It succeeded to show that the neutrinos are actually coming from the direction of the Sun. The directly following project was the SuperKamiokande experiment in 1996 where basically the main principle was retained. Although the threshold of 5 MeV was about six times higher than at Homestake, hence first of all 8 B neutrinos could be observed, about 15 events per day were detected. And this was again distinctly larger than at the radiochemical experiments. The SuperKamiokande yielded two insights. First, the measured neutrino flux of energies in the range of MeV was Φ ES (SK) = 4017 ± SNU = ( 2.42 ± ) cm 2 s 1 and therewith conform with the Kamiokande flux of 2.80 ± 0.19 ± cm 2 s 1[11]. The ration of the SSM predicted rate was still only 35.8%. These data include only the first 300 days but are already representative enough to got published in [11]. Later the last value was corrected to 46.5% [9] which is not much better. Second, a possible day/night rate asymmetry was proved but the effective discrepancy of [9] A DN = 2 Φ D Φ N Φ D + Φ N = ± wherein no significant difference could be seen. [11] As it later transpired, contrary to the fact the Earth shields 1 This reaction is also sensitive to muon and tau neutrinos which was used in the SNO experiment later. 3
4 solar neutrinos, the number of electron neutrinos at the night side is larger than on the day side which is why the Sun occurs brighter at night. Finally, the SuperKamiokande was looking for antineutrinos and the conversion probability from a solar electron neutrino to an electron anti-neutrino, respectively. They found an upper limit of 0.8% of the total flux between 8 MeV and 20 MeV predicted by the SSM [17]. 2.6 Sudbury Neutrino Observatory The Sudbury Neutrino Observatory (SNO) was the first detector explicitly searching for electron neutrinos as well as myon or tau neutrinos from the 8 B reaction. The detector was quite similar to Kamiokande but worked with heavy water D 2 O instead of light water. This allowed analysing three reaction at once. [16] First, the elastic scattering (ES) of electrons by neutrinos similar to Eq. (4) but this time explicit sensitive for all flavors of neutrinos, ν x + e ν x + e (x = e, µ, τ). (5) This reaction guarantees the Sun as source of the neutrinos. Second, a charged current (CC) reaction d + ν e p + p + e, (6) which is sensitive for electron neutrinos only. Third, a neutral-current (NC) reaction d + ν x ν x + p + n (x = e, µ, τ), (7) where a deuteron is fragmented into a proton and a neutron. This is sensitive for all types equally. This leads to the following relations between specific neutrino flux and to be measured rates, which are Φ CC = Φ e Φ ES = Φ e Φ µτ (8) Φ NC = Φ e + Φ µτ Finally, the resulting neutrino fluxes determined by SNO were [13][14] Φ total = ( ) cm 2 s 1 Φ e = (1.76 ± 0.05 ± 0.09) 10 6 cm 2 s 1 Φ µτ = ( 3.41 ± ) 10 6 cm 2 s 1. Not only the predicted total flux of 8 B neutrinos by the SSM is Φ SSM = ( ) 10 6 cm 2 s 1, and therewith very close, but also the ascertained muon and tau neutrion rate is 5.3σ above zero [13], i.e. it has to be assumed that flavor transformation exists with a probability bordering on certainty. In addition, the amount of electron neutrinos of the total flux coincides with the measurements of the former experiments, with respect to influences of the other neutrino flavors, very well. The solar neutrino problem seems to be solved. 3 Neutrino oscillations The SNO experiment has shown that neutrinos can change their flavor. One possible explanation might be neutrino oscillations. Like every particle neutrinos can be described as a wave function or a superposition of wavefunctions which is summarized by ν α = i U αi ν i. (9) We can only measure the resulting eigenstate on the left-hand side of Eq. (9), which we call flavor. It is generally accepted that there are three different flavors, namently electron, muon and tau neutrinos corresponding to the three charged leptons, i.e. α = e, µ, τ. On the right-hand side we find the mass eigenstates ν i with i = 1, 2, 3 and the mixing matrix U αi which is called the Pontecorvo-Maki-Nakagawa-Sakata (MNSP) matrix and is basically a rotation matrix with three Euler angles. It describes a charged-current interaction, i.e. a weak interaction mediated by the W boson, in the leptonic sector. [9] The assumption that only electron neutrinos are produced in the Sun is right. Now, we describe the propagation of these neutrinos in vacuum, which is given in interstellar space in good approximation, as a plane wave. Since these neutrinos are ultrahighenergetic, i.e. p m and t L, we can approximate E = p 2 + m 2 p + m2 2p E + m2 2E and it is ν i (t) = e im2 i L/2E ν i (0). (10) The eigenstates ν i are of course the mass eigenstates. But this means, that they are travel with different velocities depending on m i. The electron neutrino, as a superposition of different ν i, flows apart. Constructive interference then leads to the transition probability from flavor α to β P αβ = ν β (0) ν α (t) 2 2 = U αi Uβie im2 i L/2E. i (11) 4
5 Table 3.1: Fit values for the three-flavor neutrino oscillation parameters based on global data including solar, atmospheric, reactor and accelerator experiments. Last update Sept This is table D1 of [23]. parameter best fit 2σ 3σ m 2 21 [10 5 ev 2 ] m 2 31 [10 3 ev 2 ] sin 2 θ sin 2 θ sin 2 θ Assuming two types of neutrinos the mixing matrix U only depends on one mixing angle θ. Now, the transition probability can be written as ( m P αβ = sin 2 2θ sin 2 2 ) L, (12) 4E where m 2 = m 2 α m 2 β. According to the Standard Model of particles physics this difference would always give zero since all masses are zero. However, we can observe neutrino oscillations, so the model has to be extended. In the case of three neutrino types there are not only two parameters but at least five. Depending on possible symmetry violations there could be more. Current measurements, not only of solar neutrinos but also in particle accelerators and of atmospheric as well as reactor neutrinos, yield the values given in Tab. 3.1 by [23]. In matter scattering becomes important. As used in the SNO experiment, the cross section for elastic scattering and charged current reactions are different for electron and non-electron neutrinos. The Hamiltonian depends on the electron density and resonances occurs now. This is called the Mikheev-Smirnov- Wolfenstein (MSW) effect and is responsible for the day/night asymmetry and the energy dependence of the transistion probability. [3] 4 Current research and future questions The Solar Neutrino Problem seems to be solved. However, some questions are still of interest such as the total mass of the neutrinos or the energy dependence of neutrino oscillations. Yet, ultra-high energetic neutrinos above 5 M ev were investigated. Nevertheless, low energy neutrinos up to 2 M ev include many information. Unfortunately, a new generation of detectors is needed since these energies are below threshold for production of Čerenkov light and radiochemical reactions have too small cross sections. Also background radiation becomes important again. The 7 Be neutrinos are monoenergetic so that a time dependence can be measured well. The KamLAND 2 and Borexino 3 are supposed to research at this energy scale. And finally, pp neutrinos represent about 91% of the total neutrino flux but have a maximum energy of 0.42 MeV. Since the observation of neutrino oscillations only leads to the mass difference between two types, just a lower limit can be estimated assuming the lightest neutrino is indeed massless. An upper limit can be estimated by measuring the electron energy spectrum at the beta decay while this ends at one neutrino mass before the total energy of the system is reached. The mass of an electron antineutrino could be indicated to < 2 ev [2]. The KATRIN experiment 4 was planed to be started in 2009 and is designed to measure the mass of the electron antineutrino using the tritium beta decay to an upper limit of 0.2 ev [15]. If a neutrinoless double beta decay is possible, neutrinos would be their own antiparticles. The evidence for this decay mode is 97% (2.2σ) [22] but still in discussion since an evidence of 5σ is necessary to prove a theory. References [1] MINOS Collaboration: P. Adamson. Measurement of neutrino velocity with the minos detectors and numi neutrino beam. Physical Review D, 76:072005, [2] C. Amsler and Particle Data Group. Review of particle physics, [3] J. N. Bahcall, P. I. Krastev, and A. Yu Smirnov. Is large mixing angle msw the solution of the solar neutrino problems? Physical Review D, 60:093001, [4] John N. Bahcall. Solar neutrinos. Phys. Rev. Lett., 17(7): , [5] John N. Bahcall. How many σs is the solar neutrino effect? Phys. Rev. C, 65(1):015802, [6] John N. Bahcall, M. H. Pinsonneault, and Sarbani Basu. Solar models: current epoch and time dependences, neutrinos, and helioseismological properties, Kamioka Liquid Scintillator Antineutrino Detector 3 Boron Experiment 4 Karlsruhe Tritium Neutrino Experiment 5
6 [7] John N. Bahcall, Aldo M. Serenelli, and Sarbani Basu. New solar opacities, abundances, helioseismology, and neutrino fluxes, [8] Sarbani Basu, William J. Chaplin, Yvonne Elsworth, Roger New, and Aldo M. Serenelli. Fresh insights on the structure of the solar core, [9] Alain Bellerive. Review of solar neutrino experiments. International Journal of Modern Physics A, 19:1167, [10] B. T. Cleveland et al. Measurement of the solar electron neutrino flux with the Homestake chlorine detector. Astrophys. J., 496: , [11] The Super-Kamiokande Collabora. Measurements of the solar neutrino flux from super-kamiokande s first 300 days. ERRATUM-IBID., 81:4279, [12] DONUT Collaboration. Observation of tau neutrino interactions. Physics Letters B, 504:218, [13] SNO Collaboration. Direct evidence for neutrino flavor transformation from neutral-current interactions in the sudbury neutrino observatory. Physical Review Letters, 89:011301, [14] SNO Collaboration. Independent Measurement of the Total Active 8 B Solar Neutrino Flux Using an Array of 3 He Proportional Counters at the Sudbury Neutrino Observatory. Physical Review Letters, 101:111301, [20] S. Eidelman. Review of Particle Physics. Physics Letters B, 592:1+, [21] G. Fiorentini and B. Ricci. What have we learnt about the Sun from the measurement of the 8 B neutrino flux? Physics Letters B, 526:186, [22] H. V. Klapdor-Kleingrothaus, A. Dietz, H. L. Harney, and I. V. Krivosheina. Evidence for neutrinoless double beta decay. MOD.PHYS.LETT.A, 16:2409, [23] M. Maltoni, T. Schwetz, M. A. Tortola, and J. W. F. Valle. Status of global fits to neutrino oscillations, [24] W. Pauli. Offener Brief an die Gruppe der Radioaktiven bei der Gauvereins-Tagung zu Tübingen, [25] M. L. Perl, G. S. Abrams, A. M. Boyarski, M. Breidenbach, D. D. Briggs, F. Bulos, W. Chinowsky, J. T. Dakin, G. J. Feldman, C. E. Friedberg, D. Fryberger, G. Goldhaber, G. Hanson, F. B. Heile, B. Jean-Marie, J. A. Kadyk, R. R. Larsen, A. M. Litke, D. Lüke, B. A. Lulu, V. Lüth, D. Lyon, C. C. Morehouse, J. M. Paterson, F. M. Pierre, T. P. Pun, and P. A. Rapidis. Evidence for Anomalous Lepton Production in e + e Annihilation. Phys. Rev. Lett., 35(22): , [26] B. Pontecorvo. Lepton mixing and neutrino oscillations. J.Exptl. Theoret. Phys., 33:549, [15] The KATRIN Collaboration. Katrin design report 2004, [16] The SNO Collaboration. The sudbury neutrino observatory. NUCL.INSTRUM.METH.A, 449:172, [17] Super-Kamiokande collaboration Gando. Search for anti-electron-neutrinos from the sun at superkamiokande-i. Physical Review Letters, 90:171302, [18] C. L. Cowan, F. Reines, F. B. Harrison, H. W. Kruse, and A. D. McGuire. Detection of the free neutrino: A Confirmation. Science, 124: , [19] G. Danby. Observation of High-Energy Neutrino Reactions and the Existence of Two Kinds of Neutrinos. Phys. Rev. Lett., 9:36 44,
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text:
Hello, my name is Miles Richey
More about me
I was born in Frisco, Texas.
My eyes are hazel
I have one brother, his name is Logan, he's older.
I used to play soccer when I was younger.
I went to Wood Elementary.
I play the cello in orchestra and my brother plays the bass.
I play Football
I like to cook
My favorite kind of music is EDM
I like taking photography
One of my favorite things to do is programming like making games and stuff like that.
Some of my favorite foods are peeps, pizza, pretzels, seafood, and pie
I don't like chocolate as much as I like vanilla
I used to take taekwondo, I was a light green belt but after a year I stopped.


text:
Download Pro Speeds and Feeds apk free for Android smartphone
Posted by CamUser in Tools | Nov. 2, 2013 | 0 Comments
Apk file size: 0 bytes
Pro Speeds and Feeds comes pre loaded with all the same materials as the free version, but will allow you to add, delete and modify any and all materials. Don't like the numbers you get with the stock settings, then change them, It's that simple.
Currently supports standard square end mills making peripheral cuts.
This App may not work on all devices. Please download the free version Speeds and Feeds to test compatibility before purchasing Pro Feeds and Speeds.
Speeds and feeds is not just another milling calculator, but something much more. This calculator will give you the basic spindle RPM and feed rate based on the type of cutter and material being machined. Just tell it about your end mill, the material being cut, and max feed rate and horsepower of you CNC/machine... and Speeds and Feeds will tell you what RPM, feed rate in IPM, radial width of cut, and axial depth per pass for both roughing and finishing. All based on your machines capabilities. Feeds and Speeds will automatically adjust the feed and cut depths to stay within your specified machine horsepower. No need to look up chip loads or power factors. Speeds and Feeds is loaded with all the basic machining materials... and then some.
"This is the most useful speeds and feeds I've seen, great job"
- Mike
This is my first app and one that I made for myself. Hope it works for you too. I made this because I was looking for something portable that I could get the basic cutting info to program into my CNC without having to do allot of calculations or going through a bunch of tech sheets.
The following materials are supported.
Aluminum 6061 T1-T3, Aluminum 6061 T4-T6, Aluminum 2024, Aluminum 7075, Aluminum Billet, Aluminum Cast, Brass Free Cutting, Brass Wrought, Bronze, Copper, Iron Hard, Iron Soft, Magnesium Alloy, Plastic Acetal, Plastic Nylon, Plastic PVC, G10 Fiberglass/Polyester, Graphite, Graphite Fiber/Epoxy, Stainless 15-5 / 17-4 ph, Stainless 303, Stainless 440c, Stainless 304, Stainless 316, Steel 1018-1020, Steel 4130, Steel 4140, Steel 4340, Tool Steel A2, Tool Steel D2, Tool Steel H13, Tool Steel P20, Titanium Comm Pure, Titanium 6al-4v, Titanium 6al-6v, Inconel, Nitralloy N-315, and more.
This program gives basic feed and speed calculations. It is up to the user to determine if they are correct for each individual application and to make adjustments as needed. Use of the calculations provided may result in broken tooling and/or machine damage. Use at your own risk. No warranty is given or implied.
CamUser part of our Tools and have average installs from 100 to 500. Last Update Nov. 2, 2013. Google play rating is 82.8571. Current verison is None. Actual size 0 bytes.


text:
Kaikoura Helicopters.
Kaikoura is world renowned for its whale watching – it also boasts some of the most spectacular scenery New Zealand has to offer. Helping you experience this is Kaikoura Helicopters, the most experienced aerial whale watching company in the world. Kaikoura Helicopters also operates a number of other exciting flights including adventure trips, charters, weddings and all aspects of commercial helicopter work.
Our challenge was to develop and build a new website that showcased all of these unique experiences under the one brand that would allow Kaikoura Helicopters to promote their business to several different markets.
We used our web design and development capabilities to build a user friendly and highly visual site with targeted content for Kaikoura Helicopters' diverse customer base. Our expert web team, hosting and Search Engine Optimisation packages deliver a range of web solutions – chat to us about what we can do for you.Back to Projects