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- Dwarf_nova abstract "A U Geminorum-type variable star, or dwarf nova (pl. novae) 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 its companion. The first one to be observed was U Geminorum in 1855 however the mechanism was not known till 1974, when Brian Warner showed that the nova is due to the increase of the luminosity of the accretion disk. They are similar to classical novae in that the white dwarf is involved in periodic outbursts, but the mechanisms are different: classical novae result from the fusion and detonation of accreted hydrogen, while current theory suggests that dwarf novae result from instability in the accretion disk, when gas in the disk reaches a critical temperature that causes a change in viscosity, resulting in a collapse onto the white dwarf that releases large amounts of gravitational potential energy.Dwarf novae are distinct from classical novae in other ways; their luminosity is lower, and they are typically recurrent on a scale from days to decades. The luminosity of the outburst increases with the recurrence interval as well as the orbital period; recent research with the Hubble space telescope suggests that the latter relationship could make dwarf novae useful standard candles for measuring cosmic distances.There are three subtypes of U Geminorum star (UG):SS Cygni stars (UGSS), which increase in brightness by 2-6 mag in V in 1–2 days, and return to their original brightnesses in several subsequent days.SU Ursae Majoris stars (UGSU), which have brighter and longer "supermaxima" outbursts, or "super-outbursts," in addition to normal outbursts. Varieties of SU Ursae Majoris star include ER Ursae Majoris stars and WZ Sagittae stars.Z Camelopardalis stars (UGZ), which temporarily "halt" at a particular brightness below their peak.↑ ↑ 2.0 2.1 2.2 ↑ 3.0 3.1 ↑ ↑".
- Dwarf_nova thumbnail HTCas-LB1-2010Nov12.jpg?width=300.
- Dwarf_nova wikiPageExternalLink 30distance.
- Dwarf_nova wikiPageExternalLink 0200.pdf.
- Dwarf_nova wikiPageExternalLink messenger-no80-43-45.pdf.
- Dwarf_nova wikiPageID "5189278".
- Dwarf_nova wikiPageRevisionID "594697408".
- Dwarf_nova hasPhotoCollection Dwarf_nova.
- Dwarf_nova subject Category:Dwarf_novae.
- Dwarf_nova type CelestialBody109239740.
- Dwarf_nova type DwarfNovae.
- Dwarf_nova type NaturalObject100019128.
- Dwarf_nova type Nova109374493.
- Dwarf_nova type Object100002684.
- Dwarf_nova type PhysicalEntity100001930.
- Dwarf_nova type Star109444100.
- Dwarf_nova type Whole100003553.
- Dwarf_nova comment "A U Geminorum-type variable star, or dwarf nova (pl. novae) 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 its companion. The first one to be observed was U Geminorum in 1855 however the mechanism was not known till 1974, when Brian Warner showed that the nova is due to the increase of the luminosity of the accretion disk.".
- Dwarf_nova label "Dwarf nova".
- Dwarf_nova label "Nova enana".
- Dwarf_nova label "Nova naine".
- Dwarf_nova label "Nova nana".
- Dwarf_nova label "Nowa karłowata".
- Dwarf_nova label "Zwergnova".
- Dwarf_nova label "Карликовая новая".
- Dwarf_nova label "矮新星".
- Dwarf_nova label "矮新星".
- Dwarf_nova sameAs Zwergnova.
- Dwarf_nova sameAs Nova_enana.
- Dwarf_nova sameAs Nova_naine.
- Dwarf_nova sameAs Nova_nana.
- Dwarf_nova sameAs 矮新星.
- Dwarf_nova sameAs Nowa_karłowata.
- Dwarf_nova sameAs m.0d6zpd.
- Dwarf_nova sameAs Q244264.
- Dwarf_nova sameAs Q244264.
- Dwarf_nova sameAs Dwarf_nova.
- Dwarf_nova wasDerivedFrom Dwarf_nova?oldid=594697408.
- Dwarf_nova depiction HTCas-LB1-2010Nov12.jpg.
- Dwarf_nova isPrimaryTopicOf Dwarf_nova.
