| Revision as of 15:04, 30 October 2018 editGehenna1510 (talk | contribs)Extended confirmed users6,971 editsm CS1 error fixed← Previous edit | Revision as of 14:38, 17 August 2019 edit undoMike s (talk | contribs)Extended confirmed users21,551 edits update distance and replace refNext edit → | ||
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| | name = ] 133600}} | | name = ] 133600}} | ||
| {{Starbox observe | {{Starbox observe | ||
| | epoch = |
| epoch = J2000.0 | ||
| | equinox = ] (]) | |||
| | constell = ] | | constell = ] | ||
| | ra = {{RA|15|05|13. |
| ra = {{RA|15|05|13.2482}}<ref name="Gaia DR2"/> | ||
| | dec = {{DEC|+06|17|23. |
| dec = {{DEC|+06|17|23.6916}}<ref name="Gaia DR2"/> | ||
| | appmag_v=8.219<ref name=sb0 /> | | appmag_v = 8.219<ref name=sb0>{{cite simbad|title=HD 133600|access-date=February 3, 2011}}</ref> | ||
| }} | }} | ||
| {{Starbox character | {{Starbox character | ||
| Line 16: | Line 15: | ||
| }} | }} | ||
| {{Starbox astrometry | {{Starbox astrometry | ||
| | prop_mo_ra = |
| prop_mo_ra = {{val|−3.728|0.085}}<ref name="Gaia DR2"/> | ||
| | prop_mo_dec = |
| prop_mo_dec = {{val|−246.535|0.089}}<ref name="Gaia DR2"/> | ||
| | parallax = |
| parallax = 18.3157 | ||
| | p_error = |
| p_error = 0.0506 | ||
| | parallax_footnote = <ref name= |
| parallax_footnote = <ref name="Gaia DR2"/> | ||
| | absmag_v= 4.39<ref name=Anderson2012>{{citation | | absmag_v= 4.39<ref name=Anderson2012>{{citation | ||
| | title=XHIP: An extended hipparcos compilation | | title=XHIP: An extended hipparcos compilation | ||
| Line 30: | Line 29: | ||
| }} | }} | ||
| {{Starbox detail | {{Starbox detail | ||
| | mass= 1.00 ± 0.03 <ref name="arxiv"/> | | mass = 1.00 ± 0.03 <ref name="arxiv"/> | ||
| | radius= 1.085 | | radius = 1.085 | ||
| | luminosity_bolometric= 1.21 ± 0.14 <ref name="arxiv"/> | | luminosity_bolometric = 1.21 ± 0.14 <ref name="arxiv"/> | ||
| | luminosity_visual= ≳1.206<!--calculated from apparent magnitude without accounting for extinction (astronomy)--> | | luminosity_visual = ≳1.206<!--calculated from apparent magnitude without accounting for extinction (astronomy)--> | ||
| | temperature= {{Val|5788|6|fmt=commas}}<ref name=dosSantos2016/> | | temperature = {{Val|5788|6|fmt=commas}}<ref name=dosSantos2016/> | ||
| | metal_fe={{Val|+0.004|0.005}}<ref name=dosSantos2016/> | | metal_fe = {{Val|+0.004|0.005}}<ref name=dosSantos2016/> | ||
| | gravity={{Val|4.37|0.02}}<ref name=dosSantos2016/> | | gravity = {{Val|4.37|0.02}}<ref name=dosSantos2016/> | ||
| | rotational_velocity={{Val|1.42|0.13}}<ref name=dosSantos2016/> | | rotational_velocity = {{Val|1.42|0.13}}<ref name=dosSantos2016/> | ||
| | age_gyr= {{Val|6.57|0.46}}<ref name=dosSantos2016/> | | age_gyr = {{Val|6.57|0.46}}<ref name=dosSantos2016/> | ||
| }} | }} | ||
| {{Starbox catalog | {{Starbox catalog | ||
| | names=]+06 2987, ] 20290, ] 73815, ] 14484, ] 39253, ] 161240, ] 120828.<ref name=sb0 />}} | | names = ]+06 2987, ] 20290, ] 73815, ] 14484, ] 39253, ] 161240, ] 120828.<ref name=sb0 />}} | ||
| {{Starbox reference | {{Starbox reference | ||
| | Simbad=HD+133600}} | | Simbad = HD+133600}} | ||
| {{Starbox end}} | {{Starbox end}} | ||
| '''HD 133600''', also known as HIP 73815, is a ] ] in the ] of ].<ref name=sb0 /> It has an ] of approximately 8.219<sup>m</sup>.<ref name=sb0 /> It is similar to the Sun and has been called a near ], as it is 1.5 billion years older than the Sun.<ref>{{cite journal |last1=Ramírez |first1=I. |last2=Meléndez |first2=J. |last3=Asplund |first3=M. |title=Accurate abundance patterns of solar twins and analogs |journal=Astronomy & Astrophysics |date=12 November 2009 |volume=508 |issue=1 |pages=L17–L20 |doi=10.1051/0004-6361/200913038|bibcode=2009A&A...508L..17R }}</ref> | '''HD 133600''', also known as HIP 73815, is a ] ] in the ] of ].<ref name=sb0 /> It has an ] of approximately 8.219<sup>m</sup>.<ref name=sb0 /> It is similar to the Sun and has been called a near ], as it is 1.5 billion years older than the Sun.<ref>{{cite journal |last1=Ramírez |first1=I. |last2=Meléndez |first2=J. |last3=Asplund |first3=M. |title=Accurate abundance patterns of solar twins and analogs |journal=Astronomy & Astrophysics |date=12 November 2009 |volume=508 |issue=1 |pages=L17–L20 |doi=10.1051/0004-6361/200913038|bibcode=2009A&A...508L..17R }}</ref> | ||
| Its distance is |
Its distance is 54.6 parsecs (178 light years) from the Sun.<ref name="Gaia DR2"/> Mass is within 3 percent of the Sun.<ref name=Melendez>{{cite journal |last1=Meléndez |first1=Jorge |last2=Ramírez |first2=Iván |title=HIP 56948: A Solar Twin with a Low Lithium Abundance |journal=The Astrophysical Journal |date=10 November 2007 |volume=669 |issue=2 |pages=L89–L92 |doi=10.1086/523942|arxiv=0709.4290 |bibcode=2007ApJ...669L..89M }}</ref> | ||
| Near solar twins can help us to understand solar activity such as ]s and ] 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 ], and models of solar evolution.<ref name=Melendez/> | Near solar twins can help us to understand solar activity such as ]s and ] 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 ], and models of solar evolution.<ref name=Melendez/> | ||
| Line 55: | Line 54: | ||
| ==References== | ==References== | ||
| ⚫ | {{Reflist|refs= | ||
| ⚫ | {{Reflist |
||
| <ref name=arxiv> | <ref name=arxiv> | ||
| Line 75: | Line 73: | ||
| | year=2009 | | year=2009 | ||
| }}</ref> | }}</ref> | ||
| <ref name=dosSantos2016> | <ref name=dosSantos2016> | ||
| {{cite journal | {{cite journal | ||
| Line 91: | Line 90: | ||
| |title=The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars | |title=The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars | ||
| |journal=Astronomy & Astrophysics | |journal=Astronomy & Astrophysics | ||
| |volume=592 |pages=A156 | |volume=592 |pages=A156 | ||
| |arxiv = 1606.06214 | |arxiv = 1606.06214 | ||
| |bibcode=2016A&A...592A.156D | |bibcode=2016A&A...592A.156D | ||
| |doi=10.1051/0004-6361/201628558 | |doi=10.1051/0004-6361/201628558 | ||
| }}</ref> | }}</ref> | ||
| <ref name="Gaia DR2">{{Cite Gaia DR2|1160260989536170880}}</ref> | |||
| }} <!-- END: refs= --> | }} <!-- END: refs= --> | ||
Revision as of 14:38, 17 August 2019
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 15 05 13.2482 |
| Declination | +06° 17′ 23.6916″ |
| Apparent magnitude (V) | 8.219 |
| Characteristics | |
| Spectral type | G0 |
| B−V color index | 0.6 |
| V−R color index | 0.4 |
| R−I color index | 0.2 |
| Astrometry | |
| Proper motion (μ) | RA: −3.728±0.085 mas/yr Dec.: −246.535±0.089 mas/yr |
| Parallax (π) | 18.3157 ± 0.0506 mas |
| Distance | 178.1 ± 0.5 ly (54.6 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.39 |
| Details | |
| Mass | 1.00 ± 0.03 M☉ |
| Radius | 1.085 R☉ |
| Luminosity (bolometric) | 1.21 ± 0.14 L☉ |
| Luminosity (visual, LV) | ≳1.206 L☉ |
| Surface gravity (log g) | 4.37±0.02 cgs |
| Temperature | 5,788±6 K |
| Metallicity | +0.004±0.005 dex |
| Rotational velocity (v sin i) | 1.42±0.13 km/s |
| Age | 6.57±0.46 Gyr |
| Other designations | |
| BD+06 2987, GC 20290, HIP 73815, LTT 14484, NLTT 39253, PPM 161240, SAO 120828. | |
| Database references | |
| SIMBAD | data |
HD 133600, also known as HIP 73815, is a G-type star in the constellation of Virgo. It has an apparent visual magnitude of approximately 8.219. 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.
Its distance is 54.6 parsecs (178 light years) from the Sun. Mass is within 3 percent of the Sun.
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.
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 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
- ^ 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.
- ^ "HD 133600". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved February 3, 2011.
- 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.
- ^ 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.
- ^ 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.
- 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.
- ^ 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.
