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{{Short description|Star in the constellation Virgo}}
{{Starbox begin {{Starbox begin
| name = ] 133600}} | name = ] 133600}}
{{Starbox observe {{Starbox observe
| epoch = ] | epoch = J2000.0
| equinox = ] (])
| constell = ] | constell = ]
| ra = {{RA|15|05|13.2488}}<ref name=sb0>{{SIMBAD link|HD+133600|LTT 14484 -- High proper-motion Star}}, database entry, ]. Accessed on line February 3, 2011.</ref> | ra = {{RA|15|05|13.2482}}<ref name="Gaia DR2"/>
| dec = {{DEC|+06|17|23.676}}<ref name=sb0 /> | 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 16:
}} }}
{{Starbox astrometry {{Starbox astrometry
| prop_mo_ra = −2.40<ref name=sb0 /> | prop_mo_ra = {{val|−3.728|0.085}}<ref name="Gaia DR2"/>
| prop_mo_dec = −248.01<ref name=sb0 /> | prop_mo_dec = {{val|−246.535|0.089}}<ref name="Gaia DR2"/>
| parallax = 19.12 | parallax = 18.3157
| p_error = 1.11 | p_error = 0.0506
| parallax_footnote = <ref name=sb0 /> | parallax_footnote = <ref name="Gaia DR2"/>
| absmag_v= 4.62<ref>From apparent magnitude and parallax.</ref> | absmag_v= 4.39<ref name=Anderson2012>{{citation
| title=XHIP: An extended hipparcos compilation
| last1=Anderson | first1=E. | last2=Francis | first2=Ch.
| journal=Astronomy Letters | arxiv=1108.4971
| volume=38 | issue=5 | pages=331 | year=2012
| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
| s2cid=119257644 | postscript=. }}</ref>
}} }}
{{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&nbsp;2987, ]&nbsp;20290, ]&nbsp;73815, ]&nbsp;14484, ]&nbsp;39253, ]&nbsp;161240, ]&nbsp;120828.<ref name=sb0 />}} | names = ]+06&nbsp;2987, ]&nbsp;20290, ]&nbsp;73815, ]&nbsp;14484, ]&nbsp;39253, ]&nbsp;161240, ]&nbsp;120828.<ref name=sb0 />}}
{{Starbox reference {{Starbox reference
| Simbad=HD+133600}} | Simbad = HD+133600}}
{{Starbox end}} {{Starbox end}}


'''{{CelestialRef|HD 133600|link=no|all=show|plot=20|siblings=show|newline=yes}}''', 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>Accurate abundance patterns of solar twins and analogs. Does the anomalous solar chemical composition come from planet formation?, I. Ramírez, J. Meléndez, and M. Asplund, ''Astronomy and Astrophysics'' '''508''', #1 (December 2009), {{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 |doi-access=free }}</ref>


Its distance is 52.3 parsecs (171 light years) from the Sun. Mass is within 3 percent of the Sun.<ref name=Melendez> , Jorge Melendez and Ivan Ramırezd, ''The Astrophysical Journal'', '''669''': L89–L92, 2007 November 10. (also discusses HIP 73815, compares it with HIP 56948)</ref> 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 |s2cid=15952981 }}</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/>


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<ref name=Melendez /> 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 ]. 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<ref name=Melendez /> to show that the Sun was not unique in this respect as it has lithium abundance similar to the Sun, but is not an ideal 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 ].

{{clear}}

==Sun comparison==
This chart compares the Sun to HD 133600.

{| class="wikitable" style="text-align: center; white-space: nowrap;"
|-
!rowspan="2"| Identifier
!colspan="2"| ] Coordinates
!rowspan="2"| Distance<br>(ly)
!rowspan="2"| ]
!rowspan="2"| Temperature<br>(K)
!rowspan="2"| Metallicity<br>(dex)
!rowspan="2"| Age<br>(])
!rowspan="2"| Notes
|-
! ]
! ]
|-
|style="text-align:left;"| ]
| —
| —
| 0.00
| G2V
| 5780<ref name=apj669_2/>
| -0.01 <ref name=apj669_2/>
| 4.6
| <ref name=nssdc>{{cite web |last=Williams |first=D.R. |url=http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html |title=Sun Fact Sheet |publisher=] |year=2004 |accessdate=2009-06-23 }}</ref>
|-
|-
|style="text-align:left;"| {{CelestialRefAll|HD 133600}}
| {{RA|15|05|13.2}}
| {{DEC|+06|17|24}}
| 171
| G0
| +30
| +0.02
| +1.7
| <ref name=apj669_2/><ref name="arxiv"/>
|}

To date no solar twin with an exact match as that of the Sun has been found, however, there are some stars that come very close to being identical to that of the Sun, and are such considered solar twins by the majority of the public. An exact solar twin would be a G2V star with a 5,772K temperature, be 4.6 billion years old, with the correct metallicity and a 0.1% ] variation.<ref></ref> Stars with an age of 4.6 billion years are at the most stable state. Proper metallicity and size are also very important to low luminosity variation. <ref></ref><ref></ref><ref></ref>
]


==References== ==References==
{{Reflist|refs=


<ref name=arxiv>
{{Reflist|colwidth=30em|refs=
{{Cite journal
| last1=do Nascimento Jr | first1=J. D
| last2=Castro | first2=M
| last3=Melendez | first3=J
| last4=Bazot | first4=M
| last5=Theado | first5=S
| last6=Porto de Mello | first6=G. F
| last7=De Medeiros | first7=J. R
| title=Age and mass of solar twins constrained by lithium abundance
| journal=Astronomy & Astrophysics
| volume=501 | issue=2 | pages=687
| arxiv=0904.3580
| bibcode=2009A&A...501..687D
| doi=10.1051/0004-6361/200911935
| year=2009
| s2cid=9565600
}}</ref>


<ref name=dosSantos2016>
<ref name=apj669_2>{{cite journal | title=HIP 56948: A Solar Twin with a Low Lithium Abundance |author1=Meléndez, Jorge |author2=Ramírez, Iván | journal=The Astrophysical Journal | volume=669 | issue=2 | pages=L89–L92 |date=November 2007 | doi=10.1086/523942 | bibcode=2007ApJ...669L..89M |arxiv = 0709.4290 }}</ref>
{{cite journal
|last1=dos Santos |first1=Leonardo A.
|last2=Meléndez |first2=Jorge
|last3=Nascimento |first3=José-Dias do
|last4=Bedell |first4=Megan
|last5=Ramírez |first5=Iván
|last6=Bean |first6=Jacob L.
|last7=Asplund |first7=Martin
|last8=Spina |first8=Lorenzo
|last9=Dreizler |first9=Stefan
|last10=Alves-Brito |first10=Alan
|last11=Casagrande |first11=Luca
|date=24 August 2016
|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
|volume=592 |pages=A156
|arxiv = 1606.06214
|bibcode=2016A&A...592A.156D
|doi=10.1051/0004-6361/201628558
|s2cid=53533614
}}</ref>


<ref name="Gaia DR2">{{Cite Gaia DR2|1160260989536170880}}</ref>
<ref name=arxiv>{{Cite web| title=Age and mass of solar twins constrained by lithium abundance, January 3, 2014 | work=] | publisher=Cornell University - Astronomy & Astrophysics manuscript | url=https://arxiv.org/pdf/0904.3580v2.pdf | accessdate=July 13, 2016}}</ref>

<ref name=dosSantos2016>{{citation
| 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
| display-authors=1 | last1=dos Santos | first1=Leonardo A.
| last2=Meléndez | first2=Jorge | last3=do Nascimento | first3=José-Dias
| last4=Bedell | first4=Megan | last5=Ramírez | first5=Iván
| last6=Bean | first6=Jacob L. | last7=Asplund | first7=Martin
| last8=Spina | first8=Lorenzo | last9=Dreizler | first9=Stefan
| last10=Alves-Brito | first10=Alan | last11=Casagrande | first11=Luca
| journal=Astronomy & Astrophysics | postscript=.
| volume=592 | id=A156 | pages=8 | date=August 2016
| doi=10.1051/0004-6361/201628558 | bibcode=2016A&A...592A.156D }}</ref>


}} <!-- END: refs= --> }} <!-- END: refs= -->



{{Stars of Virgo}} {{Stars of Virgo}}


{{DEFAULTSORT:HD 133600}}
] ]
] ]
] ]
] ]
]

Latest revision as of 20:46, 17 January 2023

Star in the constellation Virgo
HD 133600
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
Distance178.1 ± 0.5 ly
(54.6 ± 0.2 pc)
Absolute magnitude (MV)4.39
Details
Mass1.00 ± 0.03  M☉
Radius1.085 R☉
Luminosity (bolometric)1.21 ± 0.14  L☉
Luminosity (visual, LV)≳1.206 L☉
Surface gravity (log g)4.37±0.02 cgs
Temperature5,788±6 K
Metallicity +0.004±0.005 dex
Rotational velocity (v sin i)1.42±0.13 km/s
Age6.57±0.46 Gyr
Other designations
BD+06 2987, GC 20290, HIP 73815, LTT 14484, NLTT 39253, PPM 161240, SAO 120828.
Database references
SIMBADdata

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 the Sun, but is not an ideal 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, S2CID 119257644.
  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. S2CID 9565600.
  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. S2CID 53533614.
  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. S2CID 15952981.
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