Gliese 268: Difference between revisions

GJ 268
Observation data; Epoch J2000 Equinox J2000
Constellation	Template:Constel
Right ascension	07h 10m 01.83458s
Declination	38° 31′ 46.0672″
Characteristics
Spectral type	M5Ve+M5Ve
Astrometry
Parallax (π)	165.2 ± 2.1 mas
Distance	19.7 ± 0.3 ly ; (6.05 ± 0.08 pc)
Other designations
	QY Aur, GJ 268, HIP 34603, AC +38 23616, G 87-26, G 07-51, LFT 512, LHS 226, LSPM J0710+3831, LTT 11987, NLTT 17470, PLX 1668, PM 07066+3838, Ross 986, TYC 2944-1956-1, 2MASS J07100180+3831457
Database references
SIMBAD	data

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Revision as of 21:29, 7 March 2015

Gliese 268 (QY Aurigae) is a RS Canum Venaticorum variable star in the Auriga constellation. RS CVn variables tend to be binary star systems with a strong magnetic field influenced by each star's rotation, which is accelerated by the tidal effects of the other star in the system.^[9] Gliese 268 in particular is composed of a binary system of two M-type dwarfs, or red dwarfs, and is one of the one hundred closest star systems to the Earth. The primary component of the system has an apparent magnitude of 12.05, and the secondary component an apparent magnitude of 12.45. Neither is visible to the naked eye from Earth.^[10]

Distance

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References

^ ^a ^b Cite error: The named reference van Leeuwen2007 was invoked but never defined (see the help page).
^ ^a ^b ^c SIMBAD, QY Aur (accessed 7 March 2015)
^ ^a ^b Cite error: The named reference van Altena1995 was invoked but never defined (see the help page).
^ Cite error: The named reference Gliese1991 was invoked but never defined (see the help page).
^ Cite error: The named reference Perryman1997 was invoked but never defined (see the help page).
^ Template:Odref
^ Template:Odref
^ Cite error: The named reference Perryman1997_tyc was invoked but never defined (see the help page).
^ "RS CVn Stars". Karl Schwarzschild Observatory. Retrieved 26 August 2011.
^ "The 100 Nearest Star Systems". Research Consortium on Nearby Stars. Georgia State University. 1 January 2011. Retrieved 26 August 2011.

Notes

This variable star–related article is a stub. You can help Wikipedia by expanding it.

This article about a red dwarf is a stub. You can help Wikipedia by expanding it.

[van_Leeuwen2007-1] Cite error: The named reference van Leeuwen2007 was invoked but never defined (see the help page).

[SIMBAD-2] SIMBAD, QY Aur (accessed 7 March 2015)

[van_Altena1995-3] Cite error: The named reference van Altena1995 was invoked but never defined (see the help page).

[Gliese1991-4] Cite error: The named reference Gliese1991 was invoked but never defined (see the help page).

[Perryman1997-5] Cite error: The named reference Perryman1997 was invoked but never defined (see the help page).

[Luyten1979_LHS-6] Template:Odref

[Luyten1979_NLTT-7] Template:Odref

[Perryman1997_tyc-8] Cite error: The named reference Perryman1997_tyc was invoked but never defined (see the help page).

[German-9] "RS CVn Stars". Karl Schwarzschild Observatory. Retrieved 26 August 2011.

[hundred-10] "The 100 Nearest Star Systems". Research Consortium on Nearby Stars. Georgia State University. 1 January 2011. Retrieved 26 August 2011.

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-'''Gliese 268''' is a [[RS Canum Venaticorum variable]] star in the [[Auriga (constellation)|Auriga]] constellation. RS CVn variables tend to be [[binary star]] systems with a strong magnetic field influenced by each star's rotation, which is accelerated by the tidal effects of the other star in the system.<ref name=German>{{cite web |url=http://www.tls-tautenburg.de/research/artie/di_rscvn.html |title=RS CVn Stars |author= |date= |work= |publisher=[[Karl Schwarzschild Observatory]] |accessdate=26 August 2011}}</ref> Gliese 268 in particular is composed of a binary system of two [[Stellar classification#Class M|M-type dwarfs]], or [[red dwarfs]], and is one of the one hundred closest star systems to the Earth. The primary component of the system has an [[apparent magnitude]] of 12.05, and the secondary component an apparent magnitude of 12.45. Neither is visible to the [[naked eye]] from Earth.<ref name=hundred>{{cite web |url=http://www.astro.gsu.edu/RECONS/TOP100.posted.htm |title=The 100 Nearest Star Systems |author= |date=1 January 2011 |work=[[Research Consortium on Nearby Stars]] |publisher=[[Georgia State University]] |accessdate=26 August 2011}}</ref>
+'''Gliese 268''' ('''QY Aurigae''') is a [[RS Canum Venaticorum variable]] star in the [[Auriga (constellation)|Auriga]] constellation. RS CVn variables tend to be [[binary star]] systems with a strong magnetic field influenced by each star's rotation, which is accelerated by the tidal effects of the other star in the system.<ref name=German>{{cite web |url=http://www.tls-tautenburg.de/research/artie/di_rscvn.html |title=RS CVn Stars |author= |date= |work= |publisher=[[Karl Schwarzschild Observatory]] |accessdate=26 August 2011}}</ref> Gliese 268 in particular is composed of a binary system of two [[Stellar classification#Class M|M-type dwarfs]], or [[red dwarfs]], and is one of the one hundred closest star systems to the Earth. The primary component of the system has an [[apparent magnitude]] of 12.05, and the secondary component an apparent magnitude of 12.45. Neither is visible to the [[naked eye]] from Earth.<ref name=hundred>{{cite web |url=http://www.astro.gsu.edu/RECONS/TOP100.posted.htm |title=The 100 Nearest Star Systems |author= |date=1 January 2011 |work=[[Research Consortium on Nearby Stars]] |publisher=[[Georgia State University]] |accessdate=26 August 2011}}</ref>
 ==Distance==