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Nova Muscae is obviously a most interesting object which will now be studied with all available means. Nova Muscae Tipo: These observations showed that the new X-ray source in Musca was most probably an exploding star a "nova" whose optical light was still brightening. A preliminary position of the X-ray source placed it in the direction of the constellation Musca within a circle with a one degree diameter. In a "classical nova", the compact star is a white dwarf star that weighs about as much as the Sun, but is no larger than the Earth.

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Subscribe Contact Site Map. The available optical and X-ray observations point to a quite unusual object. In the meantime, it had become known that also the Japanese Ginga cronimls had observed X-ray emission from the Musca region and a somewhat more croinmos position was now available. A typical nova brightens in the course of a few days to a maximum and then its light slowly decreases over a period of several weeks or months. The next night another plate with 45 min exposure and therefore showing much fainter objects was taken with the ESO Schmidt telescope by night assistant Guido Pizarro.

Cronimos - Nova Era (2014)

Preliminary observations with the ESO 3. Again, a first inspection revealed no new object in the field, brighter than magnitude 16 [2] Persisting, the astronomers then obtained a 90 min Schmidt plate in the morning of January At the La Silla Observatory, a photographic plate was exposed during 10 min with the GPO telescope in the early morning hours of January These observations showed that the new X-ray source in Musca was most probably an exploding star a "nova" whose optical light was still brightening.

At a certain moment, a thermonuclear explosion may take place cronnimos the hydrogen-rich material on the surface of the star which will blow much stellar material out into the surrounding space. The break-through and the discovery of the optical image of the X-ray emitting object was finally made in the afternoon of January ea by ESO astronomers Massimo Della Valle and Brian Jarvis. Thanks to an excellent international collaboration crinimos was discovered when it was in a cronimmos phase of transition.

At this time, and according to astronomical custom, the star was given the designation "Nova Muscae ".

Nova events are believed to occur in binary stars and to be eraa by transfer of matter from one component star to the other which is a very compact object, either a white dwarf star or a neutron star or perhaps even a "black hole ". Noting that the new source was situated far down in the southern sky and therefore not observable from Europe, Niels Lund the same evening contacted scientists at the European Southern Observatory, suggesting that a search should be made for the visible image of the X-ray emitting cronmios.

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A star of magnitude 16 is 2. They novx a number of broad emission lines from hydrogen, helium and nitrogen atoms and ions in the disk, reflecting its present, highly energetic state and also that it rotates rapidly. No X-ray fluctuations have been observed from Nova Muscae so far, but satellite observations are continuing. Contrary to a supernova explosion, the white dwarf star survives the violent event; some of these objects may actually experience repeated explosions and are known as "recurrent novae".

In X-ray novae the increase in brightness is caused by novq heating of the disk which then radiates strongly in X-ray as well as in optical light. The faintest objects which can be perceived with the unaided eye have magnitude 6. Nova Muscae Tipo: Cronimoe difference of 1 magnitude means an intensity difference of a factor 2.

It turned out that a very faint star magnitude 21 of blue colour could be seen at exactly the same position on Schmidt plates obtained in and ; it is therefore most certainly the so-called progenitor, that is, the star that exploded. About two "novae" are observed in the Milky Way Galaxy each year and some others are seen in other galaxies from time to time. That same night CCD images and spectra were obtained with the ESO New Technology Telescope and, to some surprise, it was seen that the star had brightened considerably during the preceding days; now the magnitude was almost Still, thousands of stars were seen on the Schmidt plate within the X-ray "error box" the area of uncertainty of the X-ray ceonimos.

A preliminary position of the X-ray source placed it in the direction of the constellation Musca within a circle with a one degree diameter. In a "classical nova", the compact star is a white dwarf star that weighs about as much as the Sun, but is no larger than the Earth.

Some neutron stars are detected cronimod rapidly fluctuating pulsars in supernova remnants. For more information on how ESO uses data and how you can disable cookies, please view our privacy policy.

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It now seems almost certain that it belongs to the small, select class of so-called "X-ray novae"; objects of this type have been detected in, and [3] They are different from the "classical novae" in that they emit vastly more X-ray emission; in X-ray novae the ratio between the energy emitted at X-ray and optical wavelengths is aboutwhereas for classical novae it is only 0. The brightest stars have magnitudes near O.

The dramatic increase in the brightness during the nova outburst is caused by the light emitted from the hot, expanding envelope around the binary star.

It is expected that ultraviolet spectra will be obtained with the IUE satellite. However, the present object is unusual as it began to emit X-rays, before it brightened optically.

Acting on information received from Danish scientists working with an X-ray telescope on a Soviet satellite, astronomers at the ESO La SiIla observatory in Chile have discovered a strange new star in the southern constellation of Musca the Fly.