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Symbiotic Star
A symbiotic binary is a type of binary star system, often simply called a symbiotic star. They usually contain a white dwarf with a companion red giant. The cool giant star loses material via Roche lobe overflow or through its stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as they can be used to learn about stellar evolution. They are also vital in the study of stellar wind, ionized nebulae, and accretion because of the unique interstellar dynamics present within the system. Variability Many symbiotic binaries show brightness changes and are classified as variable stars. The star Z Andromedae is often considered the prototype of the symbiotic binary class of stars. More commonly it is considered as the prototype of only a subset of symbiotic stars with irregular variations up to about 4 magnitudes in amplitude. Even the Z Andromedae variable stars are thought to be an inhomoge ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Artists Impression Of R Aquarii, A Symbiotic Star
An artist is a person engaged in an activity related to creating art, practicing the arts, or demonstrating an art. The common usage in both everyday speech and academic discourse refers to a practitioner in the visual arts only. However, the term is also often used in the entertainment business, especially in a business context, for musicians and other performers (although less often for actors). "Artiste" (French for artist) is a variant used in English in this context, but this use has become rare. Use of the term "artist" to describe writers is valid, but less common, and mostly restricted to contexts like used in criticism. Dictionary definitions The ''Oxford English Dictionary'' defines the older broad meanings of the term "artist": * A learned person or Master of Arts. * One who pursues a practical science, traditionally medicine, astrology, alchemy, chemistry. * A follower of a pursuit in which skill comes by study or practice. * A follower of a manual art, such a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Spectral Energy Distribution
A spectral energy distribution (SED) is a plot of energy versus frequency or wavelength of light (not to be confused with a 'spectrum' of flux density vs frequency or wavelength). It is used in many branches of astronomy to characterize astronomical sources. For example, in radio astronomy they are used to show the emission from synchrotron radiation, free-free emission and other emission mechanisms. In infrared astronomy, SEDs can be used to classify young stellar objects. Detector for spectral energy distribution The count rates observed from a given astronomical radiation source have no simple relationship to the flux from that source, such as might be incident at the top of the Earth's atmosphere. This lack of a simple relationship is due in no small part to the complex properties of radiation detectors. These detector properties can be divided into *those that merely attenuate the beam, including *#residual atmosphere between source and detector, *#absorption in the d ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Binary Stars
A binary star is a system of two stars that are gravitationally bound to and in orbit around each other. Binary stars in the night sky that are seen as a single object to the naked eye are often resolved using a telescope as separate stars, in which case they are called ''visual binaries''. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known. They may also be detected by indirect techniques, such as spectroscopy (''spectroscopic binaries'') or astrometry (''astrometric binaries''). If a binary star happens to orbit in a plane along our line of sight, its components will eclipse and transit each other; these pairs are called ''eclipsing binaries'', or, together with other binaries that change brightness as they orbit, ''photometric binaries''. If components in binary star systems are close enough they can gravitationally distort their mutual outer stellar atmospheres. In some cases, the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Cataclysmic Variable Stars
Cataclysm is derived from the Greek (), 'down, against', and (), 'wash over, surge'. It may refer to: Common meanings *Generally, any large-scale disaster * Deluge (mythology) *Doomsday event, see hypothetical risks to civilization, humans, and planet Earth *A catastrophic natural event: **List of geological phenomena **earthquake, the result of a sudden release of energy in the Earth's crust that creates seismic waves **volcanic eruption Video games *'' World of Warcraft: Cataclysm'', an expansion pack of Blizzard Entertainment's ''World of Warcraft'' *'' Cataclysm: Dark Days Ahead'', an open-source cross-platform roguelike video game *'' Homeworld: Cataclysm'', a stand-alone expansion, of the ''Homeworld'' space-based RTS franchise Books and comics * Cataclysm (''Dragonlance''), a fictional event in the ''Dragonlance'' novels *'' Batman: Cataclysm'', a DC Comics crossover story arc featuring Batman * '' Cataclysm: The Ultimates' Last Stand'' a 2013-2014 crossover storyline ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
University Of Exeter
, mottoeng = "We Follow the Light" , established = 1838 - St Luke's College1855 - Exeter School of Art1863 - Exeter School of Science 1955 - University of Exeter (received royal charter) , type = Public , endowment = £49.5 million , budget = £503.1 million , chancellor = Sir Michael Barber , vice_chancellor = Lisa Roberts , head_label = Visitor , head = Charles III '' ex officio'' , city = Exeter, Devon Penryn, Cornwall , country = England , coor = , administrative_staff = 2,647 , faculty = 3,145 (2020) , students = 23,613 (2018/19) , undergrad = 18,932 (2018/19) , postgrad = 4,681 (2018/19) , colours = Green and white , doctoral = , campus = Streatham – Penryn – St Luke's – , affiliations ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
IPHAS
The INT Photometric H-Alpha Survey (IPHAS) is an astronomical survey of the northern plane of our Galaxy, the Milky Way, as visible from the Isaac Newton Telescope (INT) in the Canary Islands, Spain. The survey uses two broad-band filters and a narrow H-alpha filter to obtain deep images of nebulae in our Galaxy and for identifying rare types of stars. Observations for the survey began in 2003 and are almost complete. The survey is being complemented by a sister survey of the southern Galactic Plane, VPHAS+. Once these two surveys are completed the data are expected to provide a significant leap in our knowledge of the extreme phases of stellar evolution. The goals of the survey include: * Identification of rare objects that are often characterized by strong emission in H-Alpha compared to that in broad-band filters. This includes massive OB stars, supergiants, interacting binary stars and supernova progenitors. * Mapping Galactic extinction and nebulosity. * Identifying co ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Active Galactic Nucleus
An active galactic nucleus (AGN) is a compact region at the center of a galaxy that has a much-higher-than-normal luminosity over at least some portion of the electromagnetic spectrum with characteristics indicating that the luminosity is not produced by stars. Such excess non-stellar emission has been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an "active galaxy". The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy. Active galactic nuclei are the most luminous persistent sources of electromagnetic radiation in the universe, and as such can be used as a means of discovering distant objects; their evolution as a function of cosmic time also puts constraints on models of the cosmos. The observed characteristics of an AGN depend on several properties such as the mass of the central black hole, th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astrophysical Jet
An astrophysical jet is an astronomical phenomenon where outflows of ionised matter are emitted as an extended beam along the axis of rotation. When this greatly accelerated matter in the beam approaches the speed of light, astrophysical jets become relativistic jets as they show effects from special relativity. The formation and powering of astrophysical jets are highly complex phenomena that are associated with many types of high-energy astronomical sources. They likely arise from dynamic interactions within accretion disks, whose active processes are commonly connected with compact central objects such as black holes, neutron stars or pulsars. One explanation is that tangled magnetic fields are organised to aim two diametrically opposing beams away from the central source by angles only several degrees wide Jets may also be influenced by a general relativity effect known as frame-dragging. Most of the largest and most active jets are created by supermassive black holes ( ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Long Period Variable
The descriptive term long-period variable star refers to various groups of cool luminous pulsating variable stars. It is frequently abbreviated to LPV. Types of variation The General Catalogue of Variable Stars does not define a long-period variable star type, although it does describe Mira variables as long-period variables. The term was first used in the 19th century, before more precise classifications of variable stars, to refer to a group that were known to vary on timescales typically hundreds of days. By the middle of the 20th century, long period variables were known to be cool giant stars. The relationship of Mira variables, semiregular variables, and other pulsating stars was being investigated and the term ''long period variable'' was generally restricted to the coolest pulsating stars, almost all Mira variables. Semiregular variables were considered intermediate between LPVs and Cepheids. After the publication of the General Catalogue of Variable Stars, both Mira ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mira Variable
Mira variables (named for the prototype star Mira) are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths. They are red giants in the very late stages of stellar evolution, on the asymptotic giant branch (AGB), that will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years. Mira variables are stars massive enough that they have undergone helium fusion in their cores but are less than two solar masses, stars that have already lost about half their initial mass. However, they can be thousands of times more luminous than the Sun due to their very large distended envelopes. They are pulsating due to the entire star expanding and contracting. This produces a change in temperature along with radius, both of which factors cause the variation in luminosity. The pulsation depends on the mass a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Annie Cannon
Annie Jump Cannon (; December 11, 1863 – April 13, 1941) was an American astronomer whose cataloging work was instrumental in the development of contemporary stellar classification. With Edward C. Pickering, she is credited with the creation of the Harvard Classification Scheme, which was the first serious attempt to organize and classify stars based on their temperatures and spectral types. She developed the mnemonic "Oh! Be A Fine Girl — Kiss Me!" used by students to memorize the spectral classification of stars. She was nearly deaf throughout her career after 1893, as a result of scarlet fever. She was a suffragist and a member of the National Women's Party. Personal life Cannon was born on December 11, 1863, in Dover, Delaware. She was the eldest of three daughters born to Wilson Cannon, a Delaware shipbuilder and state senator, and his second wife, Mary Jump. Cannon's mother was the first person to teach her the constellations and she encouraged her to follow her own ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
AG Draconis
AG Draconis is a binary star system in the northern constellation of Draco. It consists of a giant star and a white dwarf that revolve around each other every 550 days. Discovery AG Draconis has been catalogued since the start of the 20th century, as BD+67°922. However, its unusual nature did not start to come to light until the middle of the century. It was noted as an emission-line object in 1943, although its nature was not understood. The emission spectrum was serendipitously discovered to be variable by Nancy Grace Roman when she observed the star and found that the spectrum had completely changed since earlier observations. It was given the variable star designation AG Draconis in 1964. Variability AG Draconis spends most of its time in a quiescent phase near visual magnitude 9.8, with only small semi-regular variations thought to be due to pulsations of the giant star. At its faintest, it can reach magnitude 10.3. The semi-regular variations have per ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
