Poor Liz (original Russian: Бедная Liz) is a Russian made-for-television movie.  It was made in 2013 and first shown on television on January 2, 2014.  It is a romantic comedy.

Story
Joe Sokoloff is a sergeant in the Canadian police.  He takes a vacation to his ancestral homeland, Russia.  On his way, he his robbed while sleeping on a train.  He discovers this just as the train makes a short stop in a small town.  He sees a young woman chasing after a who had not paid for pastries he had bought from her.  Joe dashes off the train to help.  He then is taken to the police station with the man and the woman.  The local police officer wants a report.  Now Joe has missed his train. The woman takes him in while he waits for the Canadian embassy to fix things for him. Despite many comedic cultural mistakes, the woman, Liza, grows to like him.  He falls in love with her.  Liza has a daughter who is mute because of having been kidnapped earlier.  Joe is kind to the daughter, Olya.  She gradually opens up to him. She eventually regains her speech. The first step is when she sees a horse and tries to say the word.  After several times when she got mad at Joe, Liza finally understands that she loves him.  But Joe disappeared for three days after her last outburst. Olya tells Liza that Joe will return.  Then he does return.  He explains to Liza that he had to get things straightened out with the embassy.  He says he also had bought a horse and buggy.  Olya is very happy.  The three ride through town in the buggy.

Cast

Crew
Writers:Leonora Pashenko and Elena Zueva
Director: Alexsey Lisovets
Producers: Vladislav Ryashin
Executive producer: Vadim Zhuk and Larisa Zhuravskaya
Music: Vladimir Kripak and Maksim Velichko
Cinematography: Vasiliy Borodin

Actors
 Mariya Mashkova (as Liza)
 Anton Pampushnyy (as Joe)
 Niyole Seryozhnikova (as Olya)

References

Other websites
 The movie online with English subtitles:  https://www.youtube.com/watch?v=8IZc_0Q20BY

Russian movies
Television movies

Poor Liz


Sefer HaYashar, (, the Book of the Upright) is a famous treatise on Jewish ritual authored by Rabbeinu Tam, (Rabbi Jacob ben Meir, 1100–1171). The work, which survives in a somewhat incomplete and amended form, was printed in Venice in 1544 and reprinted in Vienna in 1811.

It is especially concerned with reconciling apparently contradictory decisions in different sections of the Talmud and with preserving Talmud text unchanged against those who wanted to make clever emendations.

This Sefer ha-Yashar was used a great deal by later Talmudists and introduced the form of literature called Tosafot 'Additional Notes'.

Editions
 Sefer ha-yashar (Vienna, 1811).
 Sefer ha-yashar le-rabenu Tam, ed. Simon Solomon Schlesinger (Jerusalem, 1959).  Critical edition of first section (novellae = Hebr. hiddushim).
 Sefer ha-yashar, ed. Ferdinand Rosenthal (Berlin, 1898; repr. Jerusalem, 1975).  Critical edition of second section (responsa).

External links
Jewish Encyclopedia: Jacob ben Meïr Tam: The "Sefer ha-Yashar."

12th-century books
Rabbinic legal texts and responsa
Jewish medieval literature
Treatises

Sefer haYashar (Rabbeinu Tam)


The Battle of the Sinai was one of the most consequential battles of the Yom Kippur war. An Egyptian attacking force that advanced beyond their line of defense at the Bar-Lev Line was repulsed with heavy losses by Israeli forces. This prompted the Israelis to launch Operation Abiray-Lev (Stouthearted Men) the next day, penetrating the Egyptian line of defense and crossing the Suez Canal.

Background
After Egyptian infantry had successfully crossed the canal and captured the Bar-Lev Line on October 6, Israeli forces made several counterattacks in attempts to push the Egyptians back across the Suez Canal. The Israelis suffered heavy losses in these attacks, and by October 9 Egyptian forces in the Sinai had managed to destroy 500 Israeli tanks. Following this both sides dug in. The Egyptians would not attack for fear of extending their forces beyond the cover of their SAM defences.

In the Golan Heights, Israel had repelled Syrian forces and pushed into Syria itself. By the time the Syrians, now aided by Iraqi and Jordanian expeditionary forces managed to put a halt to the Israeli advance, Israeli forces were 40 km from Damascus. Syrian president Hafez Al-Assad requested his Egyptian ally, Anwar El-Sadat, order an attack in the Sinai, which would draw Israeli attention away from the Syrian front. Sadat consented and ordered the attack. His war minister, Ahmed Ismail, and his chief of staff, Saad El Shazly, opposed the idea; Shazli in particular stated that for Egyptian forces to advance outside their SAM defences would mean their exposure to the Israeli Air Force, which the Egyptian Air Force was too weak to challenge. Sadat insisted that the attack proceed, however, and both Ahmed Ismail and Shazli had no choice but to acknowledge the order.

Prelude
The attack was to proceed on October 13, but was postponed to October 14. Four armored brigades and one mechanized infantry brigade under the command of the Second and Third Armies were to make four independent thrusts. Awaiting for them was a dug-in force of 800 Israeli tanks supported by infantry equipped with SS.11 missiles, as well as American-made LAW and TOW anti-tank missiles. Israel had in the Sinai by October 14 around fifteen brigades totaling nearly 60,000 infantry. The Israeli air force provided intense air cover during the battle.

Battle and aftermath
The Egyptians launched their offensive in the early morning of October 14, at 6:30. The mechanized infantry brigade was to attack in the direction of the Gidi Pass, one armored brigade was to attack in the direction of the Mitla Pass, one brigade was to attack towards Baluza, and two brigades were to attack in the direction of Tasa. As anticipated by many Egyptian officers, the attack was a failure. Encountering stiff Israeli resistance, the Egyptian assault came to a halt after suffering heavy losses, and Egyptian troops retreated back to their lines on the Suez Canal.

Egyptian losses in the battle were 200–250 tanks and up to 1,000 men killed and wounded in action. The 3rd Egyptian Armored Division was completely eliminated and 120 Egyptian prisoners were taken in the battle at Wadi Mab'uk. The Egyptians also lost their Second Army Commander, Saad Mamoun, who suffered a heart attack at the beginning of the day. By contrast, Israeli losses were 50–150 tanks, 60 other armored vehicles and some aircraft. The following day, the Israelis launched Operation Abiray-Lev, crossing the Suez Canal and cutting off the Egyptian Third Army's supply lines.

References

Conflicts in 1973
1973 in Egypt
Battles of the Yom Kippur War

Battle of the Sinai (1973)


William Robinson Clark  (26 March 1829 – 12 November 1912) was a Scottish-Canadian theologian.

Biography
Clark was born in Daviot, Aberdeenshire, son of Rev. James Clark. Originally educated for the Congregationalist ministry at New College London, he later conformed to the Church of England. After graduating from King's College, Aberdeen MA with honours, he went to Hertford College, Oxford. Foster's 'Alumni Oxonienses' indicates that his BA was conferred by Oxford in 1864 and his MA in 1865.

Immediately after leaving New College, London he became minister of the Congregational Church at Lymington, Hampshire. He entered the Church of England in 1856, a fact attributed by his former tutor William Farrer (1820–1908) to the influence of Clark's wife. He was the Curate of St Matthias, Birmingham, 1857–1858, and then the Dean of Taunton and prebendary of Wells Cathedral from 1859 to 1880. He was frequently selected to preach in St. Paul's Cathedral and Westminster Abbey.

In 1882, aged about 53, he emigrated to Canada and became the Professor of Mental and Moral Philosophy at Trinity College, Toronto, Ontario (from 1883 to 1908). He was noted as a lecturer and preacher. He was also Professor of Theology at Toronto University. He resigned his chair in the college in 1909, after occupying it for twenty-five years. From that date to the time of his death he held the title of Emeritus Professor and as such he sat ex officio on the Council of Trinity College.

In recognition of his services to the Church and to education he was created a Canon of St. Alban's Cathedral, the Cathedral Church of St. James (Toronto), by the third Bishop of Toronto, Arthur Sweatman. Among these services was the help he rendered in the formation of the General Synod of the Church of England in Canada, in 1893.

He was described as one of the foremost theologians in North America, and there are records of him delivering lectures in Michigan. Amongst honours and distinctions which were bestowed upon him by institutions of learning were the degrees of D.C.L., conferred by Trinity College Toronto ; D.D., conferred by Queen's University, Kingston ; and LL.D., conferred by Hobart College, Geneva, USA - now part of the Hobart and William Smith Colleges in 1888 ; his appointment by the University of Michigan as Baldwin Lecturer in 1887, and as Slocum Lecturer in 1889 ; his appointment as Honorary Professor of Hobart College, Geneva, (USA) in 1888. He was eminent in the councils of the Church of England in Canada.

He became a Fellow of the Royal Society of Canada. He was elected in 1891 and later served as President of the Society from 1899 – 1900. It seems that he was involved in the formation of the Empire Club of Canada, and became President of the Empire Club of Canada 1905 – 1906.

In Canada, he also became a close friend of the long-time Prime Minister and political figure, William Lyon Mackenzie King (1874–1950), who was also of Scottish descent, and the Reverend William Robinson Clark is referred to in the Archives of Canada.

Following his death, the Corporation of Trinity College, at its annual meeting on 21 November 1912, adopted a resolution recording the great debt of gratitude
it owed to Professor Clark. The resolution proceeded to say : —

"As a Preacher and public Lecturer, Professor Clark was very highly esteemed, and his many engagements in these capacities served to make Trinity College favourably known far and near. He showed remarkable versatility and brilliancy in his work, both in the class room and on the public platform, as well as in his literary productions, which embrace Theology, History, and Literature. Dr. Clark's singular devotion to Trinity College and the great ability with which he served it, entitle him to the lasting regard of all its supporters, while his inexhaustible human sympathy and kindness of heart ensure for him the grateful and affectionate remembrance of a host of friends."

Selected works
He was the author of many biographical and theological works (both in the UK and in Canada). Many are held in the British Library. These included:
 Self-knowledge and the four temperaments. a series of sermons preached in Lent. 1865.
 The Anglican Reformation. 1897.
 Antichrist. The First Resurrection. Two Advent sermons. 1865.
 Beveridge, the Scriptural Preacher.
 Character and Work. Hints for younger men and women. 1878.
 Christmas. [A sermon.] 1874.
 The Church and Science. 1872.
 The Comforter. [1875.]
 The Comforter: a series of sermons on certain aspects of the work of the Holy Ghost. 1864.
 Culture. [A sermon.] 1875.
 Four Advent Sermons. 1861.
 Four Sermons preached during Advent, 1860. Second edition, partially rewritten. 1861.
 The Four Temperaments; together with some occasional sermons ... Second edition. 1874.
 Hindrances to the Work of the Church in the World: a series of sermons. [Edited by W. R. Clark.] [1872.]
 The Paraclete. A series of discourses on the person and work of the Holy Spirit ... The Slocum lectures-1899; 1900.
 Pascal and the Port Royalists. 1902.
 The Prodigal Son: a series of sermons. 1860.
 The Redeemer: a series of sermons on certain aspects of the person and work of our Lord Jesus Christ. 1863.
 Righteousness exalteth a Nation. A sermon, etc. 1876.
 Savonarola: his life and times. 1880?.

References

External links

 William Robinson Clark – Obituary (RSC)

1829 births
1912 deaths
People educated at Aberdeen Grammar School
Alumni of the University of Aberdeen
Alumni of Hertford College, Oxford
Academic staff of the University of Toronto
Canadian Anglican priests
19th-century Canadian biographers
Canadian male biographers
Canadian Anglican theologians
Fellows of the Royal Society of Canada
People from Garioch
Scottish biographers
Scottish emigrants to Canada
Scottish Episcopal theologians
Church of England deans

William Robinson Clark


Battling Jane is a 1918 American silent comedy-drama film. It was directed by Elmer Clifton as a vehicle for Dorothy Gish and included some patriotic overtones. According to the Progressive Silent Film List at SilentEra.com, it is not known whether the film currently survives.

Plot
Jane, a waitress at a small-town Maine hotel, assumes guardianship of a baby whose mother has died. The baby's rakish father, Dr. Sheldon, conspires to steal prize money won by Jane after she enters the child in a baby show. Jane manages to hold the doctor and his accomplice at bay until help arrives, then uses the prize money to help the war effort by purchasing Liberty Bonds and donating the rest to the Red Cross.

Cast

Release
The film was released in the United States in September 1918, and in Canada shortly before the new year. In some venues, it was accompanied by the comedy film The Goat with Fred Stone. It would be one of the most financially successful films made by Gish for Paramount.

Battling Jane received good reviews for its performances and its scenario: "(T)hough by turns pure comedy and pure melodrama, (it) is logically and consistently told." A reviewer for the Toronto World thought Dorothy Gish "a marvel of cleverness... as charming as in any of her previous parts. Director Elmer Clifton leaves nothing to be desired, either in point of acting or investiture. The support is unusually capable." The Evening Post of Wellington, New Zealand, found the lead role "quaint"; nonetheless it praised both the "cleverly depicted" story and the leading lady: "There are hundreds of Janes in the world, no doubt... Ms. Gish portrays the character realistically."

The film played at the Strand Theatre in Christchurch, New Zealand in June 1919.

Like many American films of the time, Battling Jane was subject to cuts by city and state film censorship boards. For example, the Chicago Board of Censors required a cut, in Reel 2. of the knifing of a man in Jane's room and, in Reel 5, the last scene of a man robbing the safe.

See also
The House That Shadows Built (1931 promotional film by Paramount)

References

External links

1918 films
1918 comedy-drama films
American war comedy-drama films
American World War I propaganda films
American silent feature films
American black-and-white films
1910s English-language films
Films directed by Elmer Clifton
Films set in Maine
Paramount Pictures films
Melodrama films
1910s American films
1910s war comedy-drama films
Silent war comedy-drama films
Silent American comedy-drama films

Battling Jane


International Ultraviolet Explorer (IUE or Explorer 57, formerly SAS-D), was the first space observatory primarily designed to take ultraviolet (UV) electromagnetic spectrum. The satellite was a collaborative project between NASA, the United Kingdom's Science and Engineering Research Council (SERC, formerly UKSRC) and the European Space Agency (ESA), formerly European Space Research Organisation (ESRO). The mission was first proposed in early 1964, by a group of scientists in the United Kingdom, and was launched on 26 January 1978 aboard a NASA Thor-Delta 2914 launch vehicle. The mission lifetime was initially set for 3 years, but in the end it lasted 18 years, with the satellite being shut down in 1996. The switch-off occurred for financial reasons, while the telescope was still functioning at near original efficiency.

It was the first space observatory to be operated in real time by astronomers who visited the groundstations in the United States and Europe. Astronomers made over 104,000 observations using the IUE, of objects ranging from Solar System bodies to distant quasars. Among the significant scientific results from IUE data were the first large scale studies of stellar winds, accurate measurements of the way interstellar dust absorbs light, and measurements of the supernova SN 1987A which showed that it defied stellar evolution theories as they then stood. When the mission ended, it was considered the most successful astronomical satellite ever.

History

Motivation
The human eye can perceive light with wavelengths between roughly 350 (violet) and 700 (red) nanometres. Ultraviolet light has wavelengths between roughly 10-nm and 350-nm. UV light can be harmful to human beings, and is strongly absorbed by the ozone layer. This makes it impossible to observe UV emission from astronomical objects from the ground. Many types of object emit copious quantities of UV radiation, though: the hottest and most massive stars in the universe can have surface temperatures high enough that the vast majority of their light is emitted in the UV. Active Galactic Nuclei, accretion disks, and supernovae all emit UV radiation strongly, and many chemical elements have strong absorption lines in the UV, so that UV absorption by the interstellar medium provides a powerful tool for studying its composition.

Ultraviolet astronomy was impossible before the Space Age, and some of the first space telescopes were UV telescopes designed to observe this previously inaccessible region of the electromagnetic spectrum. One particular success was the second Orbiting Astronomical Observatory (OAO-2), which had a number of  UV telescopes on board. It was launched in 1968, and took the first UV observations of 1200 objects, mostly stars. The success of OAO-2 motivated astronomers to consider larger missions.

Conception

The orbiting ultraviolet satellite which ultimately became the IUE mission was first proposed in 1964 by British astronomer Robert Wilson. The European Space Research Organisation (ESRO) was planning a Large Astronomical Satellite (LAS), and had sought proposals from the astronomical community for its aims and design. Wilson headed a British team which proposed an ultraviolet spectrograph, and their design was recommended for acceptance in 1966.

However, management problems and cost overruns led to the cancellation of the LAS program in 1968. Wilson's team scaled down their plans and submitted a more modest proposal to ESRO, but this was not selected as the Cosmic Ray satellite was given precedence. Rather than give up on the idea of an orbiting UV telescope, they instead sent their plans to NASA astronomer Leo Goldberg, and in 1973 the plans were approved. The proposed telescope was renamed the International Ultraviolet Explorer.

Design and aims
The telescope was designed from the start to be operated in real time, rather than by remote control. This required that it would be launched into a geosynchronous orbit – that is, one with a period equal to one sidereal day of 23h 56m. A satellite in such an orbit remains visible from a given point on the Earth's surface for many hours at a time, and can thus transmit to a single ground station for a long period of time. Most space observatories in Earth orbit, such as the Hubble Space Telescope, are in a low Earth orbit in which they spend most of their time operating autonomously because only a small fraction of the Earth's surface can see them at a given time. Hubble, for example, orbits the Earth at an altitude of approximately , while a geosynchronous orbit has an average altitude of .

As well as allowing continuous communications with ground stations, a geosynchronous orbit also allows a larger portion of the sky to be viewed continuously. Because the distance from Earth is greater, the Earth occupies a much smaller portion of the sky as seen from the satellite than it does from low Earth orbit.

A launch into a geosynchronous orbit requires much more energy for a given weight of payload than a launch into low Earth orbit. This meant that the telescope had to be relatively small, with a  primary mirror, and a total weight of . Hubble, in comparison, weighs 11.1 tonnes and has a  mirror. The largest ground-based telescope, the Gran Telescopio Canarias, has a primary mirror  across. A smaller mirror means less light-gathering power, and less spatial resolution, compared to a larger mirror.

The stated aims of the telescope at the start of the mission were:

 To obtain high-resolution spectra of stars of all spectral types to determine their physical characteristics
 To study gas streams in and around binary star system
 To observe faint stars, galaxies and quasars at low resolution, interpreting these spectra by reference to high-resolution spectra
 To observe the spectra of planets and comets
 To make repeated observations of objects with variable spectrum
 To study the modification of starlight caused by interstellar dust and gas

Construction and engineering

The telescope was constructed as a joint project between NASA, ESRO (which became ESA in 1975) and the United Kingdom's SERC. SERC provided the Vidicon cameras for the spectrographs as well as software for the scientific instruments. ESA provided the solar arrays to power the spacecraft as well as a ground observing facility in Villafranca del Castillo, Spain. NASA contributed the telescope, spectrograph, and spacecraft as well as launching facilities and a second ground observatory in Greenbelt, Maryland at the Goddard Space Flight Center (GSFC).

According to the agreement setting up the project the observing time would be divided between the contributing agencies with 2/3 to NASA, 1/6 to ESA and 1/6 to the UK's SERC.

Mirror
The telescope mirror was a reflector of the Ritchey–Chrétien telescope type, which has hyperbolic primary and secondary mirrors. The primary was  across. The telescope was designed to give high quality images over a 16 arcminute field of view (about half the apparent diameter of the Sun or Moon). The primary mirror was made of beryllium, and the secondary of fused silica – materials chosen for their light weight, moderate cost, and optical quality.

Instruments

The instrumentation on board consisted of the Fine Error Sensors (FES), which were used for pointing and guiding the telescope, a high resolution and a low resolution spectrograph, and four detectors.

There were two Fine Error Sensors (FES), and their first purpose was to image the field of view of the telescope in visible light. They could detect stars down to 14th magnitude, about 1500 times fainter than can be seen with the naked eye from Earth. The image was transmitted to the ground station, where the observer would verify that the telescope was pointing at the correct field, and then acquire the exact object to be observed. If the object to be observed was fainter than 14th magnitude, the observer would point the telescope at a star that could be seen, and then apply "blind" offsets, determined from the coordinates of the objects. The accuracy of the pointing was generally better than 2 arcsecond for blind offsets

The FES acquisition images were the telescope's only imaging capability; for UV observations, it only recorded spectrum. For this, it was equipped with two spectrographs. They were called the Short Wavelength Spectrograph (SWS) and the Long Wavelength Spectrograph (LWS), and covered wavelength ranges of 115 to 200 nanometres and 185 to 330-nm respectively. Each spectrograph had both high and low resolution modes, with spectral resolutions of 0.02 and 0.60-nm respectively.

The spectrographs could be used with either of two apertures. The larger aperture was a slot with a field of view roughly 10 × 20 arcsecond; the smaller aperture was a circle about 3 arcsecond in diameter. The quality of the telescope optics was such that point sources appeared about 3 arcsecond across, so use of the smaller aperture required very accurate pointing, and it did not necessarily capture all of the light from the object. The larger aperture was therefore most commonly used, and the smaller aperture only used when the larger field of view would have contained unwanted emission from other objects.

There were two cameras for each spectrograph, one designated the primary and the second being redundant in case of failure of the first. The cameras were named LWP, LWR, SWP and SWR where P stands for prime, R for redundant and LW/SW for long/short wavelength. The cameras were television cameras, sensitive only to visible light, and light gathered by the telescope and spectrographs first fell on a UV-to-visible converter. This was a caesium-tellurium cathode, which was inert when exposed to visible light, but which gave off electrons when struck by UV photons due to the photoelectric effect. The electrons were then detected by the TV cameras. The signal could be integrated for up to many hours, before being transmitted to Earth at the end of the exposure.

Mission

Launch
The IUE was launched from Kennedy Space Center, Florida on a Thor-Delta launch vehicle, on 26 January 1978. It was launched into a transfer orbit, from which its on-board launch vehicle fired it into its planned geosynchronous orbit. The orbit was inclined by 28.6° to the Earth's equator, and had an orbital eccentricity of 0.24, meaning that the satellite's distance from Earth varied between  and . The ground track was initially centred at a longitude of approximately 70° West.

Commissioning
The first 60 days of the mission were designated as the commissioning period. This was divided into three main stages. Firstly, as soon as its instruments were switched on, the IUE observed a small number of high priority objects, to ensure that some data had been taken in the event of an early failure. The first spectrum, of the star Eta Ursae Majoris, was taken for calibration purposes three days after launch. The first science observations targeted objects including the Moon, the planets from Mars to Uranus, hot stars including Eta Carinae, cool giant stars including Epsilon Eridani, the black hole candidate Cygnus X-1, and galaxies including Messier 81 (M81) and Messier 87 (M87).

Then, the spacecraft systems were tested and optimised. The telescope was focussed, and the prime and redundant cameras in both channels were tested. It was found that the SWR camera did not work properly, and so the SWP camera was used throughout the mission. Initially, this camera suffered from significant electronic noise, but this was traced to a sensor used to align the telescope after launch. Once this sensor was switched off, the camera performed as expected. The cameras were then adjusted for best performance, and the slewing and guiding performance of the telescope evaluated and optimised

Finally, image quality and spectral resolution were studied and characterised, and the performance of the telescope, spectrographs and cameras were calibrated using observations of well-known stars. After these three phases were completed, the "routine phase" of operations began on 3 April 1978. Optimisation, evaluation and calibration operations were far from complete, but the telescope was understood well enough for routine science observations to begin.

Usage

Use of the telescope was divided between NASA, ESA and United Kingdom in approximate proportion to their relative contributions to the satellite construction: two thirds of the time was available to NASA, and one sixth each to ESA and United Kingdom. Telescope time was obtained by submitting proposals, which were reviewed annually. Each of the three agencies considered applications separately for its allocated observing time. Astronomers of any nationality could apply for telescope time, choosing whichever agency they preferred to apply to. If an astronomer was awarded time, then when their observations were scheduled, they would travel to the ground stations which operated the satellite, so that they could see and evaluate their data as it was taken. This mode of operation was very different from most space facilities, for which data is taken with no real time input from the astronomer concerned, and instead resembled the use of ground-based telescopes.

Ground support
For most of its lifetime, the telescope was operated in three eight-hour shifts each day, two from the U.S. ground station at the Goddard Space Flight Center in Maryland, and one from the ESA ground station at Villanueva de la Cañada near Madrid. Because of its elliptical orbit, the spacecraft spent part of each day in the Van Allen radiation belts, during which time science observations suffered from higher background noise. This time occurred during the second U.S. shift each day, and was generally used for calibration observations and spacecraft "housekeeping", as well as for science observations that could be done with short exposure times. The twice-daily transatlantic handovers required telephone contact between Spain and the U.S. to coordinate the switch. Observations were not coordinated between the stations, so that the astronomers taking over after the handover would not know where the telescope would be pointing when their shift started. This sometimes meant that observing shifts started with a lengthy pointing manoeuvre, but allowed maximum flexibility in scheduling of observing blocks.

Data transmission
Data was transmitted to Earth in real time at the end of each science observation. The camera read-out formed an image of 768 × 768 pixels, and the analogue-to-digital converter resulted in a dynamic range of 8 bits. The data was then transmitted to Earth via one of six transmitters on the spacecraft; four were S-band transmitters, placed at points around the spacecraft such that no matter what its attitude, one could transmit to the ground, and two were Very high frequency (VHF) transmitters, which could sustain a lower bandwidth, but consumed less power, and also transmitted in all directions. The VHF transmitters were used when the spacecraft was in the Earth's shadow and thus reliant on battery power instead of solar power.

In normal operations, observers could hold the telescope in position and wait approximately 20 minutes for the data to be transmitted, if they wanted the option of repeating the observation, or they could slew to the next target and then start the data transmission to Earth while observing the next target. The data transmitted were used for "quick look" purposes only, and full calibration was carried out by IUE staff later. Astronomers were then sent their data on magnetic tape by post, about a week after processing. From the date of the observation, the observers had a six-month proprietary period during which only they had access to the data. After six months, it became public.

Scientific results

The IUE allowed astronomers their first view of the ultraviolet light from many celestial objects, and was used to study objects ranging from Solar System planets to distant quasars. During its lifetime, hundreds of astronomers observed with IUE, and during its first decade of operations, over 1500 peer reviewed scientific articles based on IUE data were published. Nine symposia of the International Astronomical Union (IAU) were devoted to discussions of IUE results.

Solar System
All the planets in the Solar System except Mercury were observed; the telescope could not point at any part of the sky within 45° of the Sun, and Mercury's greatest angular distance from the Sun is only about 28°. IUE observations of Venus showed that the amount of sulfur monoxide and sulfur dioxide in its atmosphere declined by a large amount during the 1980s. The reason for this decline is not yet fully understood, but one hypothesis is that a large volcanic eruption had injected sulfur compounds into the atmosphere, and that they were declining following the end of the eruption.

Halley's Comet reached perihelion in 1986, and was observed intensively with the IUE, as well as with a large number of other ground-based and satellite missions. UV spectra were used to estimate the rate at which the comet lost dust and gas, and the IUE observations allowed astronomers to estimate that a total of 3×108 tons of water evaporated from the comet during its passage through the inner Solar System.

Stars
Some of the most significant results from IUE came in the studies of hot stars. A star that is hotter than about 10,000 K emits most of its radiation in the UV, and thus if it can only be studied in visible light, a large amount of information is being lost. The vast majority of all stars are cooler than the Sun, but the fraction that is hotter includes massive, highly luminous stars which shed enormous quantities of matter into interstellar space, and also white dwarf stars, which are the end stage of stellar evolution for the vast majority of all stars and which have temperatures as high as 100,000 K when they first form.

The IUE discovered many instances of white dwarf companions to main sequence stars. An example of this kind of system is Sirius, and at visible wavelengths the main sequence star is far brighter than the white dwarf. However, in the UV, the white dwarf can be as bright or brighter, as its higher temperature means it emits most of its radiation at these shorter wavelengths. In these systems, the white dwarf was originally the heavier star, but has shed most of its mass during the later stages of its evolution. Binary stars provide the only direct way to measure the mass of stars, from observations of their orbital motions. Thus, observations of binary stars where the two components are at such different stages of stellar evolution can be used to determine the relationship between the mass of stars and how they evolve.

Stars with masses of around ten times that of the Sun or higher have powerful stellar winds. The Sun loses about 10−14 solar masses per year in its solar wind, which travels at up to around , but the massive stars can lose as much as a billion times more material each year in winds travelling at several thousand kilometres per second. These stars exist for a few million years, and during this time the stellar wind carries away a significant fraction of their mass, and plays a crucial role in determining whether they explode as supernova or not. This stellar mass loss was first discovered using rocket-borne telescopes in the 1960s, but the IUE allowed astronomers to observe a very large number of stars, allowing the first proper studies of how stellar mass loss is related to mass and luminosity.

SN 1987A
In 1987, a star in the Large Magellanic Cloud exploded as a supernova. Designated SN 1987A, this event was of enormous importance to astronomy, as it was the closest known supernova to Earth, and the first visible to the naked eye, since Kepler's star in 1604 – before the invention of the telescope. The opportunity to study a supernova so much more closely than had ever been possible before triggered intense observing campaigns at all major astronomical facilities, and the first IUE observations were made about 14 hours after the discovery of the supernova.

IUE data were used to determine that the progenitor star had been a blue supergiant, where theory had strongly expected a red supergiant. Hubble Space Telescope images revealed a nebula surrounding the progenitor star which consisted of mass lost by the star long before it exploded; IUE studies of this material showed that it was rich in nitrogen, which is formed in the CNO cycle – a chain of nuclear reactions which produces most of the energy emitted by stars much more massive than the Sun. Astronomers inferred that the star had been a red supergiant, and had shed a large amount of matter into space, before evolving into a blue supergiant and exploding.

The interstellar medium
The IUE was used extensively to investigate the interstellar medium (ISM). The ISM is normally observed by looking at background sources such as hot stars or quasars; interstellar material absorbs some of the light from the background source and so its composition and velocity can be studied. One of IUE's early discoveries was that the Milky Way is surrounded by a vast halo of hot gas, known as a galactic corona. The hot gas, heated by cosmic rays and supernova, extends several thousand light years above and below the plane of the Milky Way.

IUE data was also crucial in determining how the light from distant sources is affected by dust along the line of sight. Almost all astronomical observations are affected by this interstellar extinction, and correcting for it is the first step in most analyses of astronomical spectra and images. IUE data was used to show that within the galaxy, interstellar extinction can be well described by a few simple equations. The relative variation of extinction with wavelength shows little variation with direction; only the absolute amount of absorption changes. Interstellar absorption in other galaxies can similarly be described by fairly simple "laws".

Active Galactic Nuclei
The IUE vastly increased astronomers' understanding of active galactic nuclei (AGN). Before its launch, 3C 273, the first known quasar, was the only AGN that had ever been observed at UV wavelengths. With IUE, UV spectra of AGN became widely available.

One particular target was NGC 4151, the brightest Seyfert galaxy. Starting soon after IUE's launch, a group of European astronomers pooled their observing time to repeatedly observe the galaxy, to measure variations over time of its UV emission. They found that the UV variation was much greater than that seen at optical and infrared wavelengths. IUE observations were used to study the black hole at the centre of the galaxy, with its mass being estimated at between 50 and 100 million times that of the Sun. The UV emission varied on timescales of a few days, implying that the region of emission was only a few light days across.

Quasar observations were used to probe intergalactic space. Clouds of hydrogen gas in between the Earth and a given quasar will absorb some of its emission at the wavelength of Lyman alpha. Because the clouds and the quasar are all at different distances from Earth, and moving at different velocities due to the expansion of the universe, the quasar spectrum has a "forest" of absorption features at wavelengths shorter than its own Lyman alpha emission. Before IUE, observations of this so-called Lyman-alpha forest were limited to very distant quasars, for which the redshift caused by the expansion of the universe brought it into optical wavelengths. IUE allowed nearer quasars to be studied, and astronomers used this data to determine that there are fewer hydrogen clouds in the nearby universe than there are in the distant universe. The implication is that over time, these clouds have formed into galaxies.

Ultraviolet Spectrograph Package
This experiment included the ultraviolet spectrograph package carried by the IUE, consisting of two physically distinct echelle-spectrograph/camera units capable of astronomical observations. Each spectrograph was a three-element echelle system composed of an off-axis paraboloidal collimator, an echelle grating, and a spherical first-order grating that was used to separate the echelle orders and focus the spectral display on an image converter plus SEC Vidicon camera. There was a spare camera for each unit. The camera units were able to integrate the signal. The readout/preparation cycle for the cameras took approximately 20 minutes. Wavelength calibration was provided by the use of a hollow cathode comparison lamp. The photometric calibration was accomplished by observing standard stars whose spectral fluxes had previously been calibrated by other means. Both echelle-spectrograph/camera units were capable of high-resolution (0.1 Angstrom (A)) or low-resolution (6 A) performance. The dual high/low-resolution capability was implemented by the insertion of a flat mirror in front of the echelle grating, so that the only dispersion was provided by the spherical grating. As the SEC Vidicons could integrate the signal for up to many hours, data with a signal-to-noise ratio of 50 could be obtained for B0 stars of 9th and 14th magnitudes in the high- and low-resolution modes, respectively. The distinguishing characteristic of the units was their wavelength coverage. One unit covered the wavelength range from 1192 to 1924 A in the high-resolution mode and 1135 to 2085 A in the low-resolution mode. For the other unit, the ranges were from 1893 to 3031 A and 1800 to 3255 A for the high-and low-resolution modes, respectively. Each unit also had its own choice of entrance apertures: either a 3-arcsecond hole or a 10- by 20-arcsecond slot. The 10- by 20-arcsecond slots could be blocked by a common shutter, but the 3-arcsecond aperture was always open. As a result, two aperture configurations were possible: (1) both 3-arcsecond apertures open and both 10- by 20-arcsecond slots closed, or (2) all four apertures open. With this instrumentation, the observational options open to an observer were long-wavelength and/or short-wavelength spectrograph, high or low resolution, and large or small apertures. Exposures could be made with the two spectrographs simultaneously, but the entrance apertures for each were distinct and separated in the sky by about 1 arcminute. An additional restriction was that data could be read out from only one camera at a time. However, one camera could be exposed while the other camera was being read out. The choice of high or low resolution could be made independently for the two spectrographs.

Particle Flux Monitor (Spacecraft)
The particle flux monitor experiment was placed in IUE to monitor the trapped electron fluxes that affected the sensitivity of the ultraviolet sensor in the IUE spectrograph package experiment, NSSDC ID 1978-012A-01. The particle flux monitor was a lithium-drifted silicon detector with a half-angle conical field of view of 16°. It had an aluminum absorber of 0.357 g/cm2 in front of the collimator and a brass shield with a minimum thickness of 2.31 g/cm2. The effective energy threshold for electron measurements was 1.3 MeV. The experiment was also sensitive to protons with energies greater than 15 MeV. The instrument was used as an operational tool to aid in determining background radiation and acceptable camera exposure time. The data were also useful as a monitor of the trapped radiation fluxes. The instrument was provided by Dr. C. Bostrom of the Applied Physics Laboratory of Johns Hopkins University. The instrument was turned off on 4 October 1991 because it was giving erroneous information.

Mission termination
The IUE was designed to have a minimum lifetime of three years, and carried consumable sufficient for a five-year mission. However, it lasted far longer than its design called for. Occasional hardware failures caused difficulties, but innovative techniques were devised to overcome them. For example, the spacecraft was equipped with six gyroscopes to stabilise the spacecraft. Successive failures of these in 1979, 1982, 1983, 1985 and 1996 ultimately left the spacecraft with a single functional gyroscope. Telescope control was maintained with two gyros by using the telescope's Sun sensor to determine the spacecraft's attitude, and stabilisation in three axes proved possible even after the fifth failure, by using the Sun sensor, the Fine Error Sensors and the single remaining gyroscope. Most other parts of the telescope systems remained fully functional throughout the mission.

In 1995, budget concerns at NASA almost led to the termination of the mission, but instead the operations responsibilities were redivided, with ESA taking control for 16 hours a day, and GSFC for the remaining 8 only. The ESA 16 hours was used for science operations, while the GSFC 8 hours was used only for maintenance. In February 1996, further budget cuts led ESA to decide that it would no longer maintain the satellite. Operations ceased on 30 September 1996, and all the remaining hydrazine was discharged, the batteries were drained and switched off, and at 18:44 UTC on 30 September 1996, the radio transmitter was shut down and all contact with the spacecraft was lost.

It continues to orbit the Earth in its geosynchronous orbit, and will continue to do so more or less indefinitely as it is far above the upper reaches of the atmosphere of Earth. Anomalies in the Earth's gravity due to its non-spherical shape meant that the telescope tended to drift West from its original location at approximately 70°W longitude towards approximately 110°W. During the mission, this drift was corrected by occasional rocket firings, but since the end of the mission the satellite has drifted uncontrolled to the West of its former location.

Archives
The IUE archive is one of the most heavily used astronomical archives. Data were archived from the start of the mission, and access to the archive was free to anyone who wished to use it. However, in the early years of the mission, long before the advent of the World Wide Web and fast global data transmission links, access to the archive required a visit in person to one of two Regional Data Analysis Facilities (RDAFs), one at the University of Colorado and the other at GSFC.

In 1987, it became possible to access the archive electronically, by dialling into a computer at Goddard Space Flight Center. The archive, then totalling 23 Gb of data, was connected to the computer on a mass storage device. A single user at a time could dial in, and would be able to retrieve an observation in 10–30 seconds.

As the mission entered its second decade, plans were made for its final archive. Throughout the mission, calibration techniques were improved, and the final software for data reduction yielded significant improvements over earlier calibrations. Eventually, the entire set of available raw data was recalibrated using the final version of the data reduction software, creating a uniform high quality archive. Today, the archive is hosted at the Mikulski Archive for Space Telescopes at Space Telescope Science Institute and is available via the World Wide Web and APIs.

Impact on astronomy

The IUE mission, by virtue of its very long duration and the fact that for most of its lifetime it provided astronomers' only access to UV light, had a major impact on astronomy. By the end of its mission it was considered by far the most successful and productive space observatory mission. For many years after the end of the mission, its archive was the most heavily used dataset in astronomy, and IUE data has been used in over 250 PhD projects worldwide. Almost 4,000 peer-reviewed papers have now been published based on IUE data, including some of the most cited astronomy papers of all time. The most cited paper based on IUE data is one analysing the nature of interstellar reddening, which has subsequently been cited over 5,500 times.

The Hubble Space Telescope has now been in orbit for 31 years (as of 2021) and Hubble data has been used in almost 10,000 peer-reviewed publications at that time. In 2009, the Cosmic Origins Spectrograph was installed on HST by astronauts launched with the instrument by the Space Shuttle, and this device records ultraviolet spectrum, thus proving some ultraviolet observation ability in this period. Another ultraviolet space telescope, quite different in focus, was the wide-angle imaging GALEX space telescope operated between 2003 and 2013.

Some telescope visions such as Habex or Advanced Technology Large-Aperture Space Telescope (ATLAST) have included an ultraviolet capability, although its not clear if they have any real prospects. In the 2010s, many telescope projects were struggling, and even some ground observatories saw their potential for being shut down ostensibly to save budget.

See also

 Explorer program
 Timeline of artificial satellites and space probes

References

Space telescopes
Ultraviolet telescopes
European Space Agency satellites
NASA space probes
Satellites orbiting Earth
1978 in spaceflight
Spacecraft launched in 1978

International Ultraviolet Explorer


"Lost Girl" is the second episode of the third season of the American fantasy drama series Once Upon a Time, and the show's 46th episode overall. It was first broadcast on October 6, 2013. This episode features the core characters continuing to search for Henry (Jared S. Gilmore).

Peter Pan (Robbie Kay) presents Emma Swan (Jennifer Morrison) with a map of Henry's (Jared S. Gilmore) location, though it can only be successfully used if Emma embraces her true identity. Meanwhile, Mr. Gold (Robert Carlyle) gets some startling advice; and back in fairy-tale land, the Evil Queen (Lana Parrilla) has a tempting offer for Snow White (Ginnifer Goodwin).

The episode—written by Andrew Chambliss and Kalinda Vazquez—received mixed reviews from critics, and was watched by 8.00 million people, achieving a 2.6/7 rating in 18–49 adult viewers.

Plot

Opening sequence
The Sword in the Stone is featured.

In the characters' past
After Snow White is woken up by Prince Charming and vows to take back the kingdom, the Evil Queen is tipped off by the magic mirror as to where Snow White is, and appears in the village to interrupt their plans to overthrow her. She offers an ultimatum, that Snow renounces the kingdom to her, or she will kill the people closest to her, and makes her point by choking a villager, but without killing him. Against the wishes of Charming, Snow already has an answer, leading the Prince to make a deal with Rumplestiltskin, who tells him of a legend that can be found in the Camelot realm. As they reach the destination, the two discover a sword in the stone–Excalibur. After Charming failed in his attempt to pull it, he convinces Snow to do it and she succeeds. When they return to the village, they're ready for Regina, as Snow tells her that she may be a queen, but she will not let her rule her people. Regina tries to kill Grumpy by choking him, but Snow succeeds in saving him and uses the sword to strike Regina's face. As Regina sees the scar, she warns Snow that she will meet her on the battlefield.

Hours later, Snow calls out Rumplestiltskin to ask him about Excalibur, and is willing to make a deal. As Rumplestiltskin appears, he tells her the sword is a fake–the real sword is still in Camelot–and it was Charming's idea to have her run through the sword in the stone routine. He takes her mother's necklace as payment for wasting his time. Snow returns to the campout to talk to Charming, who told her that the sword was to make her believe that she can stand up to Regina and it was all her doing without any magic. The two kiss and make up.

In Neverland
While searching for Henry, the quintet of Emma Swan, Hook, Mary Margaret, David, and Regina find themselves exhausted from hiking in the island, especially now that the island has changed a lot since Hook left. But later that night, Emma hears something and investigates, and to her surprise discovers Peter Pan, who is anxious to meet the "Savior." Emma is aware of him having Henry, but Pan has something else in mind for Emma, as he tells her that she can get her son back, but in order to do that she must follow the directions on a map that he gives her. Emma notices that the map is blank, but Pan tells her that she is the only one that can see it, and in order to do that, she has to realize what her true identity is. Pan disappears before Emma asks him more questions. As Emma tries to study the map by remembering her past, Regina looks it and casts a spell to locate Pan (since Pan was the owner of the map). Unfortunately, the directions that was to lead them to Pan was a trap, as the quintet are surrounded by The Lost Boys after Pan reminds Emma that she broke the rules (allowing Regina to cast a spell on the map), which resulted in a battle that left David slightly speared from a poisonous substance called Dreamshade, while Emma becomes spooked by the fear she saw in a Lost Boy's eyes whilst she was fighting him. Mary Margaret sees this exchange, and Emma tells her that she saw herself in the boy: it was her despair from her past as an orphan growing up without her parents. At that point the map finally reveals itself to Emma, which contains directions to a spot where Pan has placed Henry. As the team prepare to continue the search, Pan appears to Emma and compliments her for unlocking the map by admitting who she really was (an Orphan) but warns her that by the time she finds Henry, he won't want to leave. He taunts her with this message: "You won't just feel like an orphan, you'll be one." As for David, he discovers that he has been poisoned by the Dreamshade, and decides to conceal it from the others.

Meanwhile, Rumplestiltskin summons up his own shadow in an effort to bury his dagger so no one else would find it, including him. He gets a visit from an image of Belle (which he conjured up, as she was still back in Storybrooke), who reminds him that he can find Henry without resorting to becoming "The Dark One" and the only way to let go of the past is letting go of the doll (which was made by Rumple's father) that Felix gave him, and he does by throwing it over the cliff. However, the doll returns to Rumple and even his powers can't destroy it, so  Rumple decides to place it in his pocket.

Cultural references
A Star Wars allusion is noticed by Regina's use of a telekinetic chokehold; Darth Vader used a similar chokehold, as did several expanded universe Sith Lords.

Emma references the Disney film by mentioning "waxed moustache... and a perm" when talking to Hook.

When Hook threatens the Hooded Lost Boy, Felix, he makes mention of what he did to Rufio (the Lost Boy left in charge during Peter Pan's absence in the 1991 film Hook) and how his fate will be much worse.

Reception

Ratings
The episode fared successfully in ratings, achieving 8.00 million viewers, down only 0.52 viewers from the premiere episode. It became the day's top drama in Adults 18-49, scoring a 2.6/7, retaining 100% of the premiere's adult rating. The episode also ranked as the top-rated entertainment program in its hour with key women, and was the most social broadcast telecast of the evening.

Critical reception
"Lost Girl" received mixed reviews from critics.

In a review from Entertainment Weekly, Hillary Busis quotes, "Uh oh, dearies – we've reached the part in our story when everyone is being afflicted by crippling self-doubt. (Or, in Emma's case, the part where she... continues to be afflicted by crippling self-doubt.) It's a necessary step along any hero's journey. Unfortunately, it's not exactly the most scintillating subject in Once's repertoire. At least Rumbelle supporters and Captain Swan crew members each got a little something to snack on; the rest of us will just have to hope things get more exciting when Tinkerbell flits into our lives next week."

Amy Ratcliffe of IGN gave the episode a score of 6.5 out of 10; saying that "Though this episode wasn't bad, it wasn't bold. It was sleepy and comfortable, and it's too early in the season to be pulling on the plot-Snuggie. Let's hope it takes an adventurous turn next week."

Gwen Ihnat of The A.V. Club gave the episode a C− rating, saying that after seeing the storyline and pointing out that "It's criminal that most of our valuable Robert Carlyle screen time this episode is wasted on a vision and a doll." Ihnat noted that "Actually, this whole episode is moot."

References

External links

2013 American television episodes
Once Upon a Time (season 3) episodes
Television episodes directed by Ron Underwood

Lost Girl (Once Upon a Time)


The People's Civil Guard (, ) was the security force of the Communist Party of Greece (KKE) during the Greek Civil War (1946–49). It was the police counterpart of the Democratic Army of Greece (DSE), KKE's military force. It was actually the successor of the National Civil Guard, which was the successor of the Organization for the Protection of the People's Struggle (OPLA).

The People's Civil Guard included both men and women; all of them were volunteers and ideologically dedicated to the Communist Party, a situation different from that of the DSE, which engaged in forced recruitment, especially in the last stages of the Civil War.

In June 1948, the KKE leadership published a booklet to be studied by the civil guards, "Lessons of Popular Civil Guard" (, ), where it was emphasized that the Popular Civil Guard was a security force "of a new type", different from the Greek Gendarmerie and the Cities Police of the Greek government, whose aim was to serve the people.

Initially the People's Civil Guard was commanded by Stephanos Papayannis, a former Captain of the Greek Army who had joined the Communist Party during World War II, and had fought in the Greek Resistance against the Nazis; later however, Vasilis Bartziotas, a Communist Party cadre took command.

In northern Greece it was also named and it was much known as Close Self-Defense ().

References

Greek Civil War
Communist Party of Greece
1947 establishments in Greece
Defunct law enforcement agencies of Greece
Military wings of socialist parties

People's Civil Guard


MLB at Field of Dreams is a recurring Major League Baseball (MLB) regular-season game played in a ballpark adjacent to Field of Dreams in Dyersville, Iowa, a site popularized by the 1989 baseball film Field of Dreams. The first edition of the game was played on August 12, 2021, with the Chicago White Sox defeating the New York Yankees, 9–8. The second edition of the game was played August 11, 2022, with the Chicago Cubs defeating the Cincinnati Reds, 4–2. Both games were held on the second Thursday of August.

Future games are on hold while a new youth baseball and softball complex is under construction at the Field of Dreams site.

Background

The first edition of the game was planned for August 13, 2020, with the Chicago White Sox facing the New York Yankees. However, due to the COVID-19 pandemic, MLB implemented a shortened 2020 season that limited games played to each team's division and the opposite league's geographically equal division to reduce travel. Hence, on July 1, MLB announced that the St. Louis Cardinals would replace the Yankees for the game. After several St. Louis players and coaches tested positive for COVID-19 in late July, MLB postponed several Cardinals games, eventually leading the league to announce on August 3 that the MLB at Field of Dreams game would be postponed to the 2021 season. In November 2020, MLB announced the 2021 game date and that the contest would feature the originally planned participants, the White Sox and Yankees.

Ballpark

The game is hosted in Dyersville, Iowa, near the filming location of the titular 1989 baseball movie. The field constructed for the movie, which has been operated as a tourist destination since 1989, could not be brought to MLB game standards without permanently altering major features of the property and destroying its movie authenticity, so it was decided to build a separate playing facility at a distance of approximately  in the cornfields. The new field is in the property of the Ameskamp family, who used to own the left and center field of the 1988 Field of Dreams (the rest was owned by the Lansing family) before selling it to the Lansing family in 2007.

The design of the ballpark pays homage to the White Sox' home from 1910 to 1990, Comiskey Park, including the shape of the outfield and the bullpens beyond the center field fence. Windows were included in the design of the right field wall to show the cornfields beyond the ballpark and to provide views of the movie set.

Following postponement of the originally scheduled game, the field remained fallow during the 2020 season. During the 2021 season, many of the temporary structures that were intended for MLB at Field of Dreams were moved to Sahlen Field in Buffalo, New York, to allow that Triple-A ballpark to accommodate the Toronto Blue Jays. In late June 2021, a news report by KTIV of Sioux City, Iowa, showed that the baseball field and lights were in place for MLB at Field of Dreams, but seating had not yet been erected.

Games

2021 game
On August 9, it was revealed that Iowa native Pat Hoberg would be the home plate umpire for the game. The White Sox and Yankees both wore throwback uniforms resembling those worn during the 1919 Major League Baseball season. Prior to the game, a pregame ceremony was conducted, during which Kevin Costner led players from both teams onto the field from the corn, in tribute to an iconic scene which occurs in the film while Maddie Poppe sang the national anthem. Bench coach Miguel Cairo managed the White Sox as manager Tony La Russa was unavailable due to a family funeral. This was the first MLB game played in the state of Iowa. The game was called by Joe Buck (play by play), John Smoltz (analyst), Ken Rosenthal (field reporter), and Tom Verducci (field reporter) on FOX.

Recap

The early game was defined by strikeouts, with four from Lance Lynn and three from Andrew Heaney through the first two innings. The first scoring was a home run over the left field fence by José Abreu in the bottom of the first inning, the first ever major league home run hit in the state of Iowa. From the third inning on, the game was described as a slugfest with home runs by Aaron Judge in the top of the third, Eloy Jiménez in the bottom of the third, Seby Zavala in the bottom of the fourth, and Brett Gardner in the top of the sixth. In the game, there was eight total home runs hit into the cornfield. Heading into the ninth inning, the White Sox led 7–4. The Yankees then rallied ahead with a pair of two-out, two-run home runs by Aaron Judge, his second of the night, and Giancarlo Stanton, both off of Liam Hendriks, to put them ahead of the White Sox by one run. After a ground out by pinch hitter Danny Mendick and a walk to Seby Zavala, the game ended with a walk-off two-run homer hit by Tim Anderson off of Zack Britton, giving the White Sox the 9–8 win. The homer was the 15th walk-off home run against the Yankees in White Sox history; the first was hit by Shoeless Joe Jackson on July 20, 1919, a fictional version of whom features heavily in the Field of Dreams film.

Line score

Reception
Fans and media personalities alike responded positively to the presentation of the game, which drew the highest ratings for a regular-season telecast on Fox Sports at 5.9 million viewers since a Yankees–Red Sox contest on October 1, 2005. Len Kasper, who called the game on radio for the White Sox, commented that "I'm not really sure MLB could have done an event better than the Field of Dreams Game. Yes, the game was bonkers and the finish was Oscar worthy, but the entire thing—the scenery, the park, the weather, the people involved, the vibe—it was just perfect. Unforgettable experience."

2022 game

Shortly before the 2021 game, Commissioner of Baseball Rob Manfred confirmed that there would be another game at the Field of Dreams during 2022, likely during August, but did not identify which teams would be playing. MLB later announced that the Cincinnati Reds would play the Chicago Cubs at the site on August 11, 2022, with Cincinnati as the designated home team in the game. Retro-style uniforms for the teams were revealed on August 8, with the Reds' uniforms matching what the team wore in the 1919 World Series. Pre-game ceremonies began with Ken Griffey Sr. and Ken Griffey Jr. playing catch, followed by the Cubs and Reds walking in from the cornfield beyond centerfield along with multiple members of the National Baseball Hall of Fame—Johnny Bench, Andre Dawson, Ferguson Jenkins, Barry Larkin, Ryne Sandberg, and Billy Williams—and a ceremonial first pitch from Jenkins to Bench. The national anthem was sung by country singer Jessie James Decker. John Smoltz (analyst), Ken Rosenthal (field reporter), and Tom Verducci (field reporter) return to call the game with Joe Davis (play by play) calling now as the lead announcer for MLB on FOX.

Recap
Drew Smyly recorded the pitching victory for the Cubs, lasting five innings with nine strikeouts and four hits allowed. The Reds only mustered two runs, in the bottom of the seventh inning, all while having two runners on base in three separate innings and with a total of eight runners left on base. Cincinnati second baseman Jonathan India left the contest after the third inning, due to a contusion on his left leg from being hit by a pitch in the first inning; his injury later required an emergency helicopter flight to an Iowa City hospital. Chicago catcher Willson Contreras rolled his ankle rounding second base in the third inning, but remained in the game.

Line score

MiLB at Field of Dreams
On April 21, 2022, Minor League Baseball (MiLB) announced the inaugural MiLB at Field of Dreams game, a High-A contest in Dyersville between teams of the Midwest League. On August 9, the Quad Cities River Bandits hosted and defeated the Cedar Rapids Kernels, 7–2. The teams used historical franchise names for the contest, Davenport Blue Sox and Cedar Rapids Bunnies, respectively.

Future
MLB did not host a game at the ballpark in 2023 due to construction around the site. Future plans include converting the site into a youth baseball and softball complex that one day would also have a hotel. Iowa Governor Kim Reynolds confirmed that there will be another round of public funding to build a permanent stadium at the site. Former MLB player Frank Thomas, who is part of the group that owns the property, did not rule out the possibility of future MLB games at the site after 2023.

In 2024, there will be a similar game between the San Francisco Giants and St. Louis Cardinals held at Rickwood Field in Alabama.

Broadcasting
Since its inception, the game has been broadcast by Fox as part of their Thursday Night Baseball telecasts.

See also
List of neutral site regular season Major League Baseball games played in the United States and Canada
NHL Winter Classic

References

Baseball in Iowa
Dyersville, Iowa
Recurring sporting events established in 2021
Chicago Cubs
Chicago White Sox
Cincinnati Reds
New York Yankees
Field of Dreams

MLB at Field of Dreams


Michael Davis (born 19 January 1961) is a former Australian rules footballer who played with Essendon and the Sydney Swans in the Victorian Football League (VFL).

Davis, who was recruited from St Bernard's, was a rover and wingman. A left footer, Davis debuted for Essendon in their six point win over Fitzroy at Windy Hill in the 1980 VFL season. He didn't play again until 1982 and his other two appearances came in 1983, when he was also a member of Essendon's reserves premiership team. In 1984 he played one senior game for the Sydney Swans, their round nine win over Geelong.

References

1961 births
Australian rules footballers from Victoria (state)
Essendon Football Club players
Sydney Swans players
Living people

Michael Davis (Australian footballer)


The Centre Party (, , CP) was a Dutch nationalist, right-wing extremist political party espousing an anti-immigrant program. The party was founded by Henry Brookman in 1980, and was represented by Hans Janmaat in the Dutch House of Representatives from 1982, until he was expelled from the party in 1984 and joined the more moderate Centre Democrats. The CP, as well as the CD, was subject to a cordon sanitaire by the other parties in the House of Representatives. After much infighting and finally legal proceedings against the party, it was declared bankrupt in 1986. The party was soon after succeeded by the Centre Party '86, which would become increasingly radical, until it was banned in 1998.

Party history

Foundation
The Centre Party was founded on 11 March 1980 by Henry Brookman, one of the founders of the short-lived National Centre Party (NCP) in 1979 (which had been dissolved the day before the founding of the CP), and a prominent member of the Dutch People's Union (NVU). In February 1980 some radical NCP members had harassed Moroccan refugees who held a hunger strike at the Moses and Aaron church in Amsterdam. This led to a conflict within the NCP. Brookman dissolved the NCP and founded the Centre Party (CP). The party contested the 1981 elections unsuccessfully, winning just 0.1% of the vote, the same as the Dutch People's Union.

In Parliament (1982–1984)

In the 1982 election the party won 0.8% of the vote, and one seat, which was taken by Hans Janmaat. This was the first time since the Second World War that a party considered to be right-wing extremist had won a seat in parliament. Janmaat soon took over the leadership of the party, helped by the small membership of the party, his political background in mainstream political parties, and as Brookman had to move into the background due to pressure from his employer.

In the following years, the party continued its growth, and claimed 3,500 members in 1984. It was highly successful in elections, for instance winning almost 10% of the vote in the 1983 local elections in Almere, and 2.5% of the vote nationwide in the 1984 European elections.

Conflict soon erupted however, between the party leadership led by Nico Konst and Henk de Wijer, and the parliamentary section, of Janmaat and his assistants. Janmaat was accused of financial and personal improprieties, while Janmaat in turn accused the party leadership of neo-Nazi sympathies and political and organisational incompetence. While Janmaat had thought that by steering a more moderate course the CP would be able to attract more voters at the polls, he was expelled from the party by the party leadership. Janmaat then joined the recently founded Centre Democrats (CD) and kept his seat in parliament. The CP became even more isolated, and suffered from disruptive internal struggles, which were very costly. In 1986 the CP and CD organized a reconciliation meeting in Kedichem, which was turned into a disaster by radical anti-fascists. A group of these anti-fascist activists set the hotel where the meeting was located on fire, causing several heavy injuries.

The party had some moderate success in local elections of March 1986, winning 6 seats. The new optimism in the party was shattered however, when party leader Albrecht Lier defected from the party and joined the Centre Democrats in May. The CP, like the CD, was unable to obtain a seat in the 1986 election, but nevertheless won 0.4% of the vote, compared to the mere 0.1% of the CD.

Dissolution
By the 1986 election the party was disintegrating rapidly, with the party membership after the split counting a mere 100 persons, and most of the leading party members having gone over to the CD, or left politics. The party was officially declared bankrupt on 13 May 1986, after being fined a sum of money it was not able to pay. The party re-organized itself under the name Centre Party '86 (CP'86) a week later. They were never able to obtain any seats in national elections since then, and were eventually abrogated in 1998 by a Dutch court, because of the racist and xenophobic statements of its party board at a 1995 meeting. The radical neo-Nazi wing of the new party expelled the moderate nationalist wing, and several of the latter members founded the People's Nationalists Netherlands in 1997, which later became the New National Party.

Ideology
The CP saw itself as defending the rights of autochthonous Dutch people in the face of mass immigration. After it lost its parliamentary representation in 1984 the party continued in 1986 under the name Centre Party '86 and became even more radical.

The party's initial manifesto was titled "not left, not right," and combined right-wing, left-wing and green political positions. Its tenth point contained its immigration stance; "The Netherlands is not an immigrant country, so put a stop to the stream of foreigners." Together with the history of some of the party's early members, this point in the program was the main background for portraying the CP as a "right-wing extremist" party in the media. The party itself however fiercely rejected any accusations of racism and fascism.

Election results

* In 1984 the party's sole representative in parliament, Hans Janmaat, became an independent MP.

Party leaders
 Henry Brookman (1980–1982)
 Hans Janmaat (1982–1984)
 Nico Konst (1984–1985)
 Albrecht "Pim" Lier (1985–1986)
 Danny Segers (1986)

References

Bibliography

External links

1980 establishments in the Netherlands
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Conrad Charles Daellenbach C.M. (born July 12, 1945) is an American and Canadian tubist. He is best known as one of the founding members of the Canadian Brass, in which he remains the quintet's tuba player, publisher, business administrator and professional relationships manager. Daellenbach is the most recorded tuba performer in history.

Early life and personal life
Conrad Charles Daellenbach was born to a musical family in Rhinelander, Wisconsin, on July 12, 1945.  Descended from four generations of Swiss and German musicians, he followed his two older sisters into the choirs, bands and orchestras taught by his father. As a young player, Daellenbach met and studied with the legendary artist/teacher Arnold Jacobs, followed by early entry to the Eastman School of Music while still in high school, eventually graduating with a Bachelor of Music in 1966, a Master of Arts in 1968 and a Ph.D. in 1971. Daellenbach first met Arnold Jacobs at the Gunnison, Colorado Music Festival in 1962, a relationship that lasted throughout Jacobs' lifetime.

Career

Daellenbach moved to Toronto and taught music at the Faculty of Music at the University of Toronto. The Canadian Brass was formed in 1970 by Daellenbach and trombonist Gene Watts, enlisting trumpeter Stuart Laughton and University of Toronto Business School graduate Graeme Page.  At this point, Daellenbach has performed fifty years with a seven-thousand performance streak in the ensemble, often compared to the famous baseball hall-of-famer Cal Ripken Jr. who played 2632 consecutive games.

Daellenbach's contributions to the brass world include over 600 standard repertoire works for brass quintets, more than 30 best-selling concert band versions of the most popular Canadian Brass repertoire, and an educational series that has sold nearly one million copies worldwide.  His recording company, Opening Day Entertainment (ODEG), has produced over 73 CDs and DVDs.  Three ODEG CDs have been top-10 Billboard hits, four have received Juno Awards, and 13 have been Juno nominated.

Ten most defining events for Daellenbach within the Canadian Brass are:
1. Ten appearances on Sesame Street
2. Ambassadors to China in 1977 sent by Prime Minister Pierre Elliot Trudeau
3. First chamber ensemble to play the MAINSTAGE at Carnegie Hall in NYC
4. Successful appearance on the Johnny Carson Tonight Show
5. Feature artist on Hunan TV's New Year's Show viewed by over half a billion viewers 2012
6. Nominated for 17 Junos (Canadian Grammy), winner of the German Echo Award (German Grammy) and several Grammy nominations
7. Voted "Audience Favourite Tuba Player" by Brass Bulletin
8. Schweizerhof Hotel in Lucerne Switzerland designates Room 182 as the "Daellenbach Room"
9. Daellenbach invited to the Board of Euterpe Music (Toronto), honorary board memory of The Coalition for Music Education (Canada) and former board member Music Educators National Conference (USA)
10. Eastman School of Music named Dr. Daellenbach "Distinguished Alumnus."

In 2014, he was made a Member of the Order of Canada "for popularizing classical music, notably as a founder of the Canadian Brass, one of our nation's most internationally renowned classical music groups".

As of 2022, Daellenbach still plays in the Canadian Brass and, with the retirement of Gene Watts in 2010, is the last original member touring with the group.

Personal life
Daellenbach is married with two sons. The family resides in Toronto.

References

External links
 Profile at Canadian Brass's official website

1945 births
20th-century American musicians
21st-century American musicians
20th-century Canadian male musicians
21st-century Canadian male musicians
Living people
American classical tubists
American expatriates in Canada
American music educators
American people of Swiss-German descent
Canadian classical tubists
Canadian music educators
Canadian people of Swiss-German descent
Eastman School of Music alumni
Members of the Order of Canada
Musicians from Wisconsin
People from Rhinelander, Wisconsin
Academic staff of the University of Toronto
Classical musicians from Wisconsin
21st-century tubists

Charles Daellenbach