HR 511

HR 511
Observation data; Epoch J2000 Equinox J2000
Constellation	Cassiopeia
Right ascension	01h 47m 44.83s
Declination	+63° 51′ 09.0″
Apparent magnitude (V)	5.63
Characteristics
Spectral type	K0 V
U−B color index	0.41
B−V color index	0.81
Variable type	None
Astrometry
Radial velocity (Rv)	+2.8 km/s
Proper motion (μ)	RA: 582.03 mas/yr ; Dec.: −246.86 mas/yr
Parallax (π)	100.24 ± 0.68 mas
Distance	32.5 ± 0.2 ly ; (9.98 ± 0.07 pc)
Absolute magnitude (MV)	5.64
Details
Mass	0.85 M☉
Radius	0.83 R☉
Luminosity	0.53 L☉
Temperature	5420 K
Metallicity	95.5%
Rotation	21.67 days (2 km/s)
Age	2.3-4 × 109 years
Other designations
	GJ 75, HR 511, BD +63°238, HD 10780, LHS 1297, LTT 10619, GCTP 371.00, SAO 11983, HIP 8362.
Database references
SIMBAD	data

HR 511 (also designated Gliese 75 among others) is an orange dwarf of spectral type K0V in the constellation Cassiopeia. The star is relatively close, 32.5 light years from the Sun.

This star is estimated to be about the same age as the sun. It has not been identified as a member of any moving star groups. This star has displayed unusual emissions of Ca II and is much more x-ray luminous than the Sun. It is considered a relatively active star.^[3] Based on an iron abundance of [-0.02], the metallicity of this star appears to be similar to that of the Sun.^[4]

References

^ H. M. Johnson, C. D. Wright (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series. 53: 643–711. doi:10.1086/190905.
^ Approximating the star as a black body, then R_{HR 511} / R_Sun = (T_Sun/T_{HR 511})² × ( L_{HR 511} / L_Sun )^0.5 = 1.14 × 0.73 = 0.83
^ ^a ^b ^c ^d ^e E. J. Gaidos, G. W. Henry, S. M. Henry (2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". The Astronomical Journal. 120 (2): 1006–1013. doi:10.1086/301488. Retrieved 2008-09-14.{{cite journal}}: CS1 maint: multiple names: authors list (link)
^ ^a ^b S. Feltzing, G. Gonzalez (2001). "The nature of super-metal-rich stars. Detailed abundance analysis of 8 super-metal-rich star candidates". Astronomy and Astrophysics. 367: 253–265. doi:10.1051/0004-6361:20000477. Retrieved 2006-08-18.

External links

"ARICNS 4C00155". ARI Data Base for Nearby Stars. Astronomisches Rechen-Institut. March 4, 1998. Retrieved 2008-02-27.
SolStation

[1] H. M. Johnson, C. D. Wright (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series. 53: 643–711. doi:10.1086/190905.

[2] Approximating the star as a black body, then R_{HR 511} / R_Sun = (T_Sun/T_{HR 511})² × ( L_{HR 511} / L_Sun )^0.5 = 1.14 × 0.73 = 0.83

[gaidos-3] E. J. Gaidos, G. W. Henry, S. M. Henry (2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". The Astronomical Journal. 120 (2): 1006–1013. doi:10.1086/301488. Retrieved 2008-09-14.{{cite journal}}: CS1 maint: multiple names: authors list (link)

[metal-4] S. Feltzing, G. Gonzalez (2001). "The nature of super-metal-rich stars. Detailed abundance analysis of 8 super-metal-rich star candidates". Astronomy and Astrophysics. 367: 253–265. doi:10.1051/0004-6361:20000477. Retrieved 2006-08-18.

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