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	Cataclysmic variable star - Wikipedia, the free encyclopedia
		Cataclysmic variables (also U Geminorum Stars) are a class of binary stars containing a white dwarf and a companion star.
		The companion star is usually a red dwarf, although in some cases it is another white dwarf or a slightly evolved star (subgiant).
		Cataclysmic variables are subdivided into several smaller groups, often presented by a bright prototype star characteristic of the class.
	en.wikipedia.org /wiki/Cataclysmic_variable_star (477 words)

	Variable Star - Slackerpedia Galactica
		The primary way variable stars are studied is by measurement of their light curve -- a graph of their apparent brightness measured as a function of time.
		Variable stars were one of the earliest classes of object to help usher in the field of astrophysics -- the study of astronomical objects with an eye towards understanding the physics of their behavior.
		There are several dozen classes and subclasses of variable star, and although there are often common reasons for the observed variability (like accretion from one star to another in a binary, or pulsations) the behavior of a specific class is unique, and provides insight into the behavior of the object.
	www.slackerastronomy.org /slackerpedia/index.php/Variable_Star (813 words)

	AAVSO: TT Arietis, January 2002 Variable Star Of The Month
		While the most common explanation for emanating X-rays from non-magnetic cataclysmic variables is that this is the form radiation emitted at the boundary layer region between the white dwarf and the disk, analysis of the hard X-ray spectrum suggests that these events are not produced in the outer part of the accretion disk.
		It is unclear whether the VY Scl behavior is common property of all cataclysmic variables with orbital periods near the 2-3 hour period gap and may be an evolutionary effect, or whether it is a property of the class of novalike variables clumped in the 3-4 hours period region (Shafter et al.
		SU UMa stars are seen to undergo two distinct types of outbursts: while one is faint, frequent, and short with a duration of 1 to 2 days, the other (referred to as a "superoutburst") is bright, less frequent, and long with a duration of 10 to 20 days.
	www.aavso.org /vstar/vsots/0102.shtml (2977 words)

	Binary and Variable Stars (Site not responding. Last check: 2007-10-09)
		A variable star, on the other hand, is a star that, for one reason of another, changes its luminosity in either a predictable pattern or at random.
		Binary stars are important in stellar science because it is only when a star is in a binary system that we have the possibility of deriving its true mass.
		RR Lyrae stars are a sub-classification of Cepheid variables.
	filer.case.edu /~sjr16/advanced/stars_binvar.html (1239 words)

	Iowa Robotic Telescope Facilities
		Cataclysmic variable stars (also known as eruptive variables) generally consist of a contact binary system in which mass is being transferred from a cool M-type star to a white dwarf.
		As the stars pass in front of one another, the light from the background star is obscured, causing a temporary and often dramatic decrease in the amount of light received from these stars.
		Variables are divided into four main classes: pulsating and eruptive, where the variability is due to physical changes in the star or star system, and eclipsing binary and rotating stars, where the variability is due to an eclipse of one star by another, or the effect of stellar rotation.
	www-astro.physics.uiowa.edu /research/projects.html (1092 words)

	Variable star Summary (Site not responding. Last check: 2007-10-09)
		Variable stars are stars that have regular or semi-regular, periodically varying brightnesses, and they have been known since medieval times.
		Variable stars of this type only occur when the binary star system is properly aligned for the observer to see one member being eclipsed by the other.
		Cepheid variable stars are pulsating variables that possess a very significant characteristic; in the early 1900s Henrietta Leavitt and Harlow Shapley found that the speed at which they pulsate is directly related to the their brightness.
	www.bookrags.com /Variable_star (4064 words)

	Cataclysmic Variable Stars: Modern Astronomy in Motion
		Cataclysmic variable stars (CVs) are binary star systems containing a low-mass main sequence secondary and a white dwarf primary star.
		In cataclysmic variables, a red dwarf is transferring matter onto a white dwarf.
		Outbursts are the result of two possible occurrences: the sudden transfer of matter from the secondary star or an instability in the accretion disk.
	members.wri.com /jeffb/poster/poster.html (601 words)

	The Astrophysics Spectator: Types of Cataclysmic Variable
		Despite this, cataclysmic variables display a rich variety of behavior that is a manifestation of three pieces of physics: the accretion disk surrounding the degenerate dwarf, the interaction of accreting gas with the magnetic field of the degenerate dwarf, and the nuclear fusion of hydrogen and helium accumulated at the surface of the degenerate dwarf.
		Instead, the gas is forced by the magnetic field to flow to the star's magnetic poles, where it passes through a standing shock wave in the star's atmosphere, releasing its gravitational potential energy as visible and x-ray light.
		These cataclysmic variables are characterized by their outbursts of energy rather than by the characteristics of their light.
	www.astrophysicsspectator.com /topics/stars/BinaryCVType.html (1112 words)

	[No title]
		The star, known as GK Persei (or GK Per for short), brightens by a factor of 15 or so every three or four years, but the time of these outbursts is not exactly predictable.
		One of the stars is a magnetic white dwarf, a dead star.
		Stars like GK Per are believed to undergo classical nova outbursts every 10,000 years although GK Per may be unique as it is thought the 1901 explosion may have been the first by this pair of stars.
	heasarc.gsfc.nasa.gov /docs/xte/whatsnew/ras_press_release.txt (897 words)

	vik dhillon: research (Site not responding. Last check: 2007-10-09)
		Cataclysmic variables are a vital link in the evolutionary chain of binary stars, coming immediately after a common-envelope phase and evolving via magnetic braking and gravitational radiation - observations of cataclysmic variables have played a key role in the development of these theories.
		If one of the stars in a close binary is a white dwarf, and the other is a star which is in contact with its Roche lobe, then the system is known as a cataclysmic variable.
		We review infrared (1-2.5 micron) observations of cataclysmic variables, a relatively unexplored part of the spectrum in which the dominant sources of emission are the secondary star, the outer regions of the accretion disc and the accretion column in magnetic systems.
	www.shef.ac.uk /physics/people/vdhillon/research.html (1265 words)

	Hubble Heritage Archive - 2003
		These stars represent an ideal situation to study star formation history, for there are young, hot, blue stars near the center, while older, cooler, red stars are more evenly spread.
		Comparing the brightness of all the stars in the images, the astronomers were able to identify several cataclysmic variable stars in the cluster.
		The most massive stars in the region are over 120 times the sun's mass and posseses surface temperatures as high as 40,000 K (72,000 °F).
	filer.case.edu /~sjr16/advanced/archive_hst_2003.html (3275 words)

	The Discoverer of U Geminorum
		It is evidently a variable star of a very interesting description, inasmuch as the minimum brightness appears to extend over a great part of the whole period, contrary to what happens with Algol and S Cancri.
		R Lep was christened "Hind’s Crimson Star" after he wrote in October 1845: "of the most intense crimson, resembling a blood-drop on the background of the sky".
		Long term and perhaps more importantly, his early discovery of U Gem means that today astronomers have historical data on a cataclysmic variable star over a period of 150 years and it will always be 40 years longer than for any other similar class of star.
	home.mindspring.com /~mikesimonsen/cvnet/id34.html (1273 words)

	AAVSO: SS Cyg, June 2000 Variable Star Of The Month
		Being the brightest of the stars of its dwarf nova class, there is no doubt that SS Cyg is a favorite of many observers.
		Pickering noted as "an unusually large range for a variable having so short a period." This new variable was assigned the name SS Cyg in 1897; a name that has become well known and revered in the astronomical community.
		Due to the evolution of the system, the main sequence star loses matter which is streamed in the direction of the primary, forming an accretion disk around the white dwarf star.
	www.aavso.org /vstar/vsots/0600.shtml (2724 words)

	APOD: 2006 February 24 - Recurrent Nova RS Ophiuci (Site not responding. Last check: 2007-10-09)
		Explanation: This pretty star field in the constellation Ophiucus is centered on a star not often seen - RS Ophiuci.
		A type of cataclysmic variable star classified as a recurrent nova, RS Oph dramatically increased in brightness from 11th magnitude, too faint to appear on some star charts.
		Such stars are now modeled as interacting binary star systems, composed of a compact white dwarf star co-orbiting with a swollen red giant.
	antwrp.gsfc.nasa.gov /apod/ap060224.html (230 words)

	Archived Research Projects
		Research on variable stars is important because it provides information about stellar properties such as mass, radius, luminosity, temperature, internal and external structure, composition, and evolution.
		By studying the position of these stars in the galaxy (requiring knowledge of their location in the sky and their distance from us) as well as of their velocity in the galaxy, we can learn about the structure of the galaxy and its formation history.
		Once each star has been assigned a spectral type, they can be compared with a template of the appropriate spectral type for which the radial velocity is very precisely known (see figure 2), and the distance can be derived from known relationships between the spectral type and absolute luminosity of these stars.
	www.astro.washington.edu /premap/projects_archive.php (1438 words)

	HubbleSite - NewsCenter - Hubble Probes the Workings of a Stellar Hydrogen Bomb (05/22/1995) - Release Images
		This is an illustration of a class of double star called a cataclysmic variable.
		The system consists of a white dwarf star - a dense, burned-out star that has collapsed to the size of Earth and a companion that is a normal star, similar to but smaller than the Sun.
		The stars are so close together gas flows from the normal star onto the dwarf where it swirls into a pancake-shaped disk.
	hubblesite.org /newscenter/archive/releases/1995/23/image/a (210 words)

	Spectroscopy of quasars
		The red line lies between the image of the bright red supergiant star in the cluster, and the position where its spectrum would start if it were in fact a hot, blue star.
		However, it is a cool, red star, and its spectrum is deficient in the shorter wavelengths; the yellow line shows where the spectrum of this red star actually begins.
		It is clear that the red star is relatively lacking in short wavelengths, and is relatively brighter at longer wavelengths.
	www.physics.adelaide.edu.au /~pmcgee/starspec.htm (456 words)

	SS Cygni.... Cataclysmic Variable Star in Cygnus
		SS Cyg is a cataclysmic variable star in CYGNUS, the Swan.
		In this case the known star counts and magnitudes refer to the comparison star.
		For counts 45806 of the known star of magnitude 9.9, and counts of SS Cyg 17703, then the resultant magnitude for ss cyg is 10.9
	sunra.lbl.gov /~vhoette/SSCyg (495 words)

	A Beginner's Guide to Cataclysmic Variables
		In a CV binary, one star is a white dwarf: a collapsed star with the mass of the Sun in the volume of the Earth (our Sun will become a white dwarf in about four and a half billion years).
		The red star in a CV is so close to the white dwarf that it becomes tidally distorted --- gas is stripped off the red star and falls towards the white dwarf.
		The difference between the nova-like variables and dwarf novae is that nova-like variables don't undergo dwarf nova outbursts.
	www.mssl.ucl.ac.uk /www_astro/gal/cv_beginners.html (1980 words)

	EF Eridani - Wikipedia, the free encyclopedia
		EF Eridani (abbreviated EF Eri, sometimes incorrectly referred to as EF Eridanus) is a variable star of the type known as polars, AM Herculis stars, or magnetic cataclysmic variable stars.
		The star system consists of a white dwarf star with a substellar massed former star in orbit.
		The substellar mass in orbit around the white dwarf is a star which lost all of its gas to the white dwarf, except what remains, a 0.05 solar mass ball, which is too small to continue fusion, and does not have the composition of a super-planet, brown dwarf, or white dwarf.
	en.wikipedia.org /wiki/EF_Eridani (232 words)

	Jul 23, 2005 UT: MV Lyr
		This star is currently being monitored by the Center for Backyard Astrophysics.
		MV Lyr is the star near differential mag 0.5, with an elevated scatter.
		If we can continue to include this star in the field while monitoring MV Lyr, we might be able to answer a few of the questions Lew Cook raises in his report on photometry of V0449 Lyrae.
	spiff.rit.edu /richmond/ritobs/jul22_2005/jul22_2005.html (1075 words)

	Stars and The Milky Way @ Gary's Astronomy Homework Help
		Astronomy 162: Stars, Galaxies, and Cosmology @ Univ. of Tenn.
		Stars evolved past that are found in the lower right as white dwarfs.
		Astronomy 162: Stars, Galaxies, and Cosmology University of Tennessee, Knoxville.
	www.members.aol.com /gca7sky/stars.htm (5122 words)

	HubbleSite - NewsCenter - Hubble Probes the Workings of a Stellar Hydrogen Bomb (05/22/1995) - Introduction
		Each dwarf - dense, burned-out stars that have collapsed to the size of Earth - is in a compact binary system, called a cataclysmic variable, where its companion is a normal star similar to, but smaller than the Sun.
		The stars are so close together that the entire binary system would fit inside the Sun.
		Their closeness allows gas to flow from the normal star onto the dwarf, where it swirls into a pancake-shaped disk [see illustration].
	hubblesite.org /newscenter/archive/releases/1995/23 (183 words)

	Cataclysmic Variables
		One type of binary that might form this way is a "cataclysmic variable" (CV), a pairing of a normal, hydrogen-burning star and a burned-out star called a white dwarf.
		I'm studying, through time-series CCD photometry, this particularly interesting group of variable stars, as an active member of the Center for Backyard Astrophysics, headed by Columbia University professor Joe Patterson.
		I'm author and co-author of an extensive set of articles on cataclysmic variables.
	users.skynet.be /fa079980/cataclysmic_variables.htm (245 words)

	APOD Index - Stars: Binary Stars
		In a binary system, the higher mass star will evolve faster and will eventually become a compact object - either a white dwarf star, a neutron star, or fl hole.
		Some stars are members of close binary systems where material from one star swirls around the other in an accretion disk.
		The brighter yellow star is itself a binary star system, but too close together to be resolved even with a telescope.
	antwrp.gsfc.nasa.gov /apod/binary_stars.html (436 words)

	Stellar Astrophysics at Penn State
		Wade and collaborators carried out a study of the ultraviolet spectra of accretion disks in cataclysmic variables, with emphasis on limb darkening.
		In the latter case, there are noticeable changes in the shapes of lines from highly ionized species and in the ratio of lines formed at high and low temperature, so high quality line profiles obtained in the UV may serve as a diagnostic of the structure of the disk.
		Eracleous and collaborators have been studying the periodic oscillations and large aperiodic flares of the cataclysmic variable AE Aquarii using ultraviolet spectra obtained with the HST.
	www.astro.psu.edu /research/stellar_group.html (1688 words)

	SS Cygni.... Cataclysmic Variable Star in Cygnus
		This way the star is always enclosed in the circle made by the aperture tool around the star.
		C1 is for the counts of SS Cyg and C2 is for the comparison star counts.
		Comparison Stars and Calculating Magnitude Reference for an image of SS Cyg taken with the Yerkes Rooftop North 10 inch telescope.
	hou.lbl.gov /~vhoette/Explorations/SSCyg (1055 words)

	Amateurs Help Astronomers Unravel A Propeller Star
		On August 30-August 31, 2005 two space-based and four professional ground-based observatories are scheduled to observe the cataclysmic variable star AE Aqr.
		Such simultaneous multiwavelength coverage is required to provide the clearest picture of the locations, mass motions, energetics, and inter-relationships of the various emission regions in the star.
		AE Aqr is an intermediate polar, a type of cataclysmic variable star.
	www.physorg.com /news6040.html (405 words)

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