HD 133600

HD 133600, also known as HIP 73815, is a G-type star in the constellation of Virgo.[2] It has an apparent visual magnitude of approximately 8.219m.[2] It is similar to the Sun and has been called a near solar twin, as it is 1.5 billion years older than the Sun.[6]

HD 133600
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Virgo
Right ascension  15h 05m 13.2482s[1]
Declination +06° 17′ 23.6916″[1]
Apparent magnitude (V) 8.219[2]
Characteristics
Spectral type G0[2]
B−V color index 0.6[2]
V−R color index 0.4[2]
R−I color index 0.2[2]
Astrometry
Proper motion (μ) RA: −3.728±0.085[1] mas/yr
Dec.: −246.535±0.089[1] mas/yr
Parallax (π)18.3157 ± 0.0506[1] mas
Distance178.1 ± 0.5 ly
(54.6 ± 0.2 pc)
Absolute magnitude (MV)4.39[3]
Details
Mass1.00 ± 0.03 [4] M☉
Radius1.085 R☉
Luminosity (bolometric)1.21 ± 0.14 [4] L☉
Luminosity (visual, LV)≳1.206 L☉
Surface gravity (log g)4.37±0.02[5] cgs
Temperature5,788±6[5] K
Metallicity [Fe/H]+0.004±0.005[5] dex
Rotational velocity (v sin i)1.42±0.13[5] km/s
Age6.57±0.46[5] Gyr
Other designations
BD+06 2987, GC 20290, HIP 73815, LTT 14484, NLTT 39253, PPM 161240, SAO 120828.[2]
Database references
SIMBADdata

Its distance is 54.6 parsecs (178 light years) from the Sun.[1] Mass is within 3 percent of the Sun.[7]

Near solar twins can help us to understand solar activity such as solar flares and sunspot cycles over longer time periods than the historical records, and to put unique historical events such as the Maunder minimum in context. They can also be used to set the zero point of fundamental calibrations in astrophysics, and models of solar evolution.[7]

Near solar twins can also help answer whether the Sun is unique or not. It used to be thought that the Sun might be unique for its low lithium abundance. This star was one of two stars that were used in 2007 papers by Melendez & Ramırez[7] to show that the Sun was not unique in this respect as it has lithium abundance similar to our Sun, but is not an idea comparison as HD 133600 is 1.5 billion years older than the Sun. Yet, this has made it a useful star for studies into the problem of the depleted lithium abundance at the solar surface compared with other stars, something that is not yet fully understood, and known as the Lithium depletion problem.

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. "HD 133600". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved February 3, 2011.
  3. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  4. do Nascimento Jr, J. D; Castro, M; Melendez, J; Bazot, M; Theado, S; Porto de Mello, G. F; De Medeiros, J. R (2009). "Age and mass of solar twins constrained by lithium abundance". Astronomy & Astrophysics. 501 (2): 687. arXiv:0904.3580. Bibcode:2009A&A...501..687D. doi:10.1051/0004-6361/200911935.
  5. dos Santos, Leonardo A.; Meléndez, Jorge; Nascimento, José-Dias do; Bedell, Megan; Ramírez, Iván; Bean, Jacob L.; Asplund, Martin; Spina, Lorenzo; Dreizler, Stefan; Alves-Brito, Alan; Casagrande, Luca (24 August 2016). "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars". Astronomy & Astrophysics. 592: A156. arXiv:1606.06214. Bibcode:2016A&A...592A.156D. doi:10.1051/0004-6361/201628558.
  6. Ramírez, I.; Meléndez, J.; Asplund, M. (12 November 2009). "Accurate abundance patterns of solar twins and analogs". Astronomy & Astrophysics. 508 (1): L17–L20. Bibcode:2009A&A...508L..17R. doi:10.1051/0004-6361/200913038.
  7. Meléndez, Jorge; Ramírez, Iván (10 November 2007). "HIP 56948: A Solar Twin with a Low Lithium Abundance". The Astrophysical Journal. 669 (2): L89–L92. arXiv:0709.4290. Bibcode:2007ApJ...669L..89M. doi:10.1086/523942.
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