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Nova Reticuli 2020
YZ Reticuli, also known as Nova Reticuli 2020 was a naked eye nova in the constellation Reticulum discovered on July 15, 2020. Previously it was known as a Super_soft_X-ray_source#VY_Scl_cataclysmic_variables, VY Sculptoris type object with the designation MGAB-V207. VY Sculptoris type The variability of the object was first discovered by an amateur astronomer, Gabriel Murawski, and reported on August 6, 2019 with the name MGAB-V207. Archive photometry data from the Catalina Real-time Transient Survey and All Sky Automated Survey for SuperNovae, ASAS-SN showed nova-like (NL) brightness variations between Magnitude_(astronomy), magnitudes 15.8 and 17.0, exhibiting a deep dimming event in late 2006. The spectrum shows a Subdwarf_B_star, hot subdwarf (sdB) or a white dwarf origin, which is consistent with VY Scl type objects. Nova eruption On July 15, 2020 Robert H. McNaught discovered a bright Transient astronomical event, transient (Magnitude_(astronomy), magnitude 5.3) ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Reticulum (constellation)
Reticulum is a small, faint constellation in the southern sky. Its name is Latin for a small net, or reticle—a net of crosshairs at the focus of a telescope eyepiece that is used to measure star positions. The constellation is best viewed between October and December, and save for one main star visible in ideal conditions, cannot be seen from north of the 30th parallel north. History A constellation in this area was introduced by Isaac Habrecht II in his celestial globe in 1621, who named it ''Rhombus''. It was replaced with a somewhat different constellation by the French astronomer Nicolas Louis de Lacaille in the eighteenth century; during his stay at the Cape of Good Hope, he named the constellation le Réticule Rhomboide to commemorate the reticle in his telescope eyepiece. The name was later Latinized to Reticulum in his star catalogue ''Coelum Australe Stelliferum''. In 1810, the stars of Reticulum were used by William Croswell to produce the constellation '' Marmor Sc ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Southern African Large Telescope
The Southern African Large Telescope (SALT) is a 10-metre class optical telescope designed mainly for spectroscopy. It consists of 91 hexagonal mirror segments each with a 1-metre inscribed diameter, resulting in a total hexagonal mirror of 11.1 by 9.8 m. It is located close to the town of Sutherland in the semi-desert region of the Karoo, South Africa. It is a facility of the South African Astronomical Observatory, the national optical observatory of South Africa. SALT is the largest optical telescope in the southern hemisphere. It enables imaging, spectroscopic, and polarimetric analysis of the radiation from astronomical objects out of reach of northern hemisphere telescopes. It is closely based on the Hobby-Eberly Telescope (HET) at McDonald Observatory, with some changes in its design, especially to the spherical aberration corrector. The main driver for these changes were desired improvements to the telescope's field of view. It shares the same fixed mirror altitude ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
The Astronomical Journal
''The Astronomical Journal'' (often abbreviated ''AJ'' in scientific papers and references) is a peer-reviewed monthly scientific journal owned by the American Astronomical Society (AAS) and currently published by IOP Publishing. It is one of the premier journals for astronomy in the world. Until 2008, the journal was published by the University of Chicago Press on behalf of the AAS. The reasons for the change to the IOP were given by the society as the desire of the University of Chicago Press to revise its financial arrangement and their plans to change from the particular software that had been developed in-house. The other two publications of the society, the ''Astrophysical Journal'' and its supplement series, followed in January 2009. The journal was established in 1849 by Benjamin A. Gould. It ceased publication in 1861 due to the American Civil War, but resumed in 1885. Between 1909 and 1941 the journal was edited in Albany, New York. In 1941, editor Benjamin Boss arrange ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Novae In The Milky Way Galaxy
This is a partial list of novae in the Milky Way galaxy that have been discovered and recorded since 1891. Novae are stars that undergo dramatic explosions, but unlike supernovae, these do not result in the destruction of the original star. The likely rate of novae in the Milky Way is about 40 per year,Prialnik, Dina. "Novae", pp. 1846-56, in Paul Murdin, ed. ''Encyclopedia of Astronomy and Astrophysics.'' London: Institute of Physics Publishing Ltd and Nature Publishing Group, 2001. but of these only about 10 per year are discovered by observers as of the 2000s (decade).CBAT List of Novae in the Milky Way discovered since 1612 This list attempts to include only the brighter or more notable novae. The |
Superhump
In astronomy, a superhump is a periodic brightness variation in a cataclysmic variable star system, with a period within a few percent of the orbital period of the system. History Superhumps were first seen in SU Ursae Majoris (SU UMa) stars, a subclass of dwarf novae, at times when the binary system underwent a superoutburst, which is an unusually strong outburst (increase in brightness) caused by an increased accretion rate. Period excess The period of the superhump variations can be either greater or less than the orbital period, known as positive or negative superhumps respectively. The period excess is the difference between the superhump period and the orbital period, expressed as a fraction of the orbital period. Physical origin The accretion disk is elongated by the tidal force of the donor star. The elliptical disk precesses around the white dwarf accretor over a time interval much longer than the orbital period, the beat period, causing a slight change in the orien ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
V392 Persei
V392 Persei, also known as Nova Persei 2018, is a bright nova in the constellation Perseus discovered on April 29, 2018. It was previously known as a dwarf nova. Dwarf nova A ''U Geminorum-type variable star'' or ''dwarf nova'' is a type of cataclysmic variable star consisting of a close binary star system in which one of the components is a white dwarf that accretes matter from a cool main sequence or subgiant companion. V392 Persei was discovered in 1970 and received its variable star designation a year later. It is normally visual magnitude 17.4 and experiences outbursts of 2-3 magnitudes. Its spectrum in the quiescent state has been studied and only the cool star is detected. The spectrum shows emission lines of hydrogen-alpha (Hα) and both neutral and ionised helium. The brightest recorded observations is at magnitude 5.6. Nova eruption On April 29, 2018 it was discovered by ''Yuji Nakamura'' to be extremely bright, and it was spectroscopically conf ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
V407 Cygni
V4 or V-4 may refer to: Science and technology * LNER Class V4, a British steam locomotive * V4 engine, a V engine with four cylinders in two banks of two cylinders * Visual area V4, in the visual cortex * Klein four-group, in mathematics * V.4, an ITU-T recommendation for data transmission * ATC code V04 ''Diagnostic agents'', a subgroup of the Anatomical Therapeutic Chemical Classification System * The V4 JavaScript engine for QML * V4, one of six precordial leads in electrocardiography Other uses * Visegrád Group, an alliance of four Central European states - Czech Republic, Hungary, Poland and Slovakia * ''Rheinbote'' or V-4, a German World War II four-stage missile * Saint Kitts & Nevis (ITU prefix) * Vieques Air Link (IATA airline code) * V4, a grade (climbing) for difficulty of a boulder climbing route See also *4V (other) 4V or 4-V may refer to: *4V, abbreviation for 4 volts *4V, abbreviation for 4-valve engine *4V, IATA code for Birdy Airlines *Venera 4 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
AAVSO
The American Association of Variable Star Observers (AAVSO) is an international nonprofit organization, founded in 1911, focused on coordinating, analyzing, publishing, and archiving variable star observations made largely by amateur astronomers. The AAVSO creates records that establish light curves depicting the variation in brightness of a star over time, and makes them available to professional astronomers, researchers, and educators. Since professional astronomers do not have the time or the resources to monitor every variable star, astronomy is one of the few sciences where amateurs can make genuine contributions to scientific research. During 2011, the 100th year of the AAVSO's existence, the 20-millionth variable star observation was received into the database. The AAVSO International Database (AID) stores over 35 million observations as of 2019. The organization receives nearly 1,000,000 observations annually from around 2,000 professional and amateur observers and is quot ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
The Astronomer's Telegram
''The Astronomer's Telegram'' (''ATel'') is an internet-based short-notice publication service for quickly disseminating information on new astronomical observations. Examples include gamma-ray bursts, gravitational microlensing, supernovae, novae, or X-ray transients, but there are no restrictions on content matter. Telegrams as available instantly on the service's website and distributed to subscribers via email digest within 24 hours. ''The Astronomer's Telegram'' was launched on 17 December 1997 by Robert E. Rutledge with the goal of rapidly (<1 s) sharing information of interest to astronomers. Telegrams are sent out daily by email, but especially time sensitive events can be transmitted instantly. Since 2013, information is also broadcast over Twitter and Facebook. To publish, astronomers request credentials. Credentials are issued to professional astronomers and graduate students, after verification by personal contact. Once credentials have been supplied and telegrams ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Nova Sagittarii 1991
A nova (plural novae or novas) is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star (hence the name "nova", which is Latin for "new") that slowly fades over weeks or months. Causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars. All observed novae involve white dwarfs in close binary systems. The main sub-classes of novae are classical novae, recurrent novae (RNe), and dwarf novae. They are all considered to be cataclysmic variable stars. Classical nova eruptions are the most common type. They are likely created in a close binary star system consisting of a white dwarf and either a main sequence, subgiant, or red giant star. When the orbital period falls in the range of several days to one day, the white dwarf is close enough to its companion star to start drawing accreted matter onto the surface of the white dwarf, which creates a dense but shallow atmosphere. This atmo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Siding Spring 2
Siding may refer to: * Siding (construction), the outer covering or cladding of a house * Siding (rail) A siding, in rail terminology, is a low-speed track section distinct from a running line or through route such as a main line, branch line, or spur. It may connect to through track or to other sidings at either end. Sidings often have lighte ..., a track section See also * {{disambiguation fr:Parement nl:Parement ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
P Cygni Profile
P Cygni (34 Cygni) is a variable star in the constellation Cygnus. The designation "P" was originally assigned by Johann Bayer in ''Uranometria'' as a nova. Located about 5,300 light-years (1,560 parsecs) from Earth, it is a hypergiant luminous blue variable (LBV) star of spectral type B1-2 Ia-0ep that is one of the most luminous stars in the Milky Way. Visibility The star is located about 5,000 to 6,000 light-years (1,500–1,800 parsecs) from Earth. Despite this vast distance, it is visible to the naked eye in suitable dark sky locations. It was unknown until the end of the 16th century, when it suddenly brightened to 3rd magnitude. It was first observed on 18 August (Gregorian) 1600 by Willem Janszoon Blaeu, a Dutch astronomer, mathematician and globe-maker. Bayer's atlas of 1603 assigned it the miscellaneous label P and the name has stuck ever since. After six years the star faded slowly, dropping below naked-eye visibility in 1626. It brightened again in 1655, bu ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
