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}}
}}
{{Starbox detail
{{Starbox detail
| source = <ref name=Fuhrmann2012/>
| source = <ref name=Rains2020/>
| component1 = χ Eri A
| component1 = A
| mass = 1.58
| mass = 1.58<ref name=Fuhrmann2012/>
| radius = {{Val|4.06|0.16}}
| radius = {{Val|3.993|0.027}}
| luminosity = 392<ref name=Mcdonald2012/>
| luminosity = {{val|9.84|0.39}}
| temperature = {{Val|5135|80|fmt=commas}}
| temperature = {{Val|5115|49|fmt=commas}}
| gravity = {{Val|3.42|-0.10}}
| gravity = {{Val|3.42|0.10}}
| metal_fe = {{Val|−0.18|0.07}}
| metal_fe = {{Val|−0.18|0.07}}
| rotational_velocity = {{Val|2.0|1.0}}
| rotational_velocity = 4.50
| age_myr =
| age_myr =
}}
}}
{{Starbox catalog
{{Starbox catalog
| names = χ Eri, [[Catalogues of Fundamental Stars|FK5]] 68, [[Gliese Catalogue of Nearby Stars|GJ]] 81, [[Henry Draper Catalogue|HD]] 11937, [[Hipparcos Catalogue|HIP]] 9007, [[Bright Star Catalogue|HR]]&nbsp;566, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 232573.<ref name=SIMBAD/>
| names = {{odlist | B=χ Eri | FK5=68 | GJ=81 | HD=11937 | HIP=9007 | HR=566 | SAO=232573 }}<ref name=SIMBAD/>
}}
}}
{{Starbox reference
{{Starbox reference
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}}
}}
{{Starbox end}}
{{Starbox end}}

'''χ Eridani''' (Latinised as '''Chi Eridani''') is a [[binary star]]<ref name=Eggleton2008/> system in the [[constellation]] [[Eridanus (constellation)|Eridanus]]. It is visible to the naked eye with an [[apparent visual magnitude]] of 3.70.<ref name=Mermilliod1986/> The distance to this system, as determined using the [[stellar parallax|parallax method]], is around 58&nbsp;[[light year]]s.<ref name=vanLeeuwen2007/> The pair had an [[angular separation]] of 5.0&nbsp;[[arcsecond]]s as of 1994. This corresponds to a [[projected separation]] of around 128&nbsp;[[Astronomical Unit|AU]].<ref name=Poveda1994/>
'''χ Eridani''' (Latinised as '''Chi Eridani''') is a [[binary star]]<ref name=Eggleton2008/> system in the [[constellation]] [[Eridanus (constellation)|Eridanus]]. It is visible to the naked eye with an [[apparent visual magnitude]] of 3.70.<ref name=Mermilliod1986/> The distance to this system, as determined using the [[stellar parallax|parallax method]], is around 58&nbsp;[[light year]]s.<ref name=vanLeeuwen2007/> The pair had an [[angular separation]] of 5.0&nbsp;[[arcsecond]]s as of 1994. This corresponds to a [[projected separation]] of around 128&nbsp;[[Astronomical Unit|AU]].<ref name=Poveda1994/>


The primary component is an [[stellar evolution|evolving]] [[G-type star|G-type]] [[subgiant]] star with a [[stellar classification]] of G8&nbsp;IV.<ref name=Torres2006/> It is about 1.6 times the mass of the Sun and has 4 times the Sun's radius.<ref name=Fuhrmann2012/> The star shines with 392<ref name=Mcdonald2012/> times the [[solar luminosity]] from its [[stellar atmosphere|outer atmosphere]] at an [[effective temperature]] of 5,135&nbsp;K.<ref name=Fuhrmann2012/> Unusually for a star of this class, it shows a [[Photometry (astronomy)|photometric]] [[Variable star|variability]] of 0.04 in magnitude, which may be due to a previous mass transfer from the secondary companion, or else from an undiscovered third companion.<ref name=Fuhrmann2012/>
The primary component is an [[stellar evolution|evolving]] [[G-type star|G-type]] [[subgiant]] star with a [[stellar classification]] of G8&nbsp;IV.<ref name=Torres2006/> It is about 1.6 times the mass of the Sun and has 4 times the Sun's radius.<ref name=Fuhrmann2012/> The star shines with 10 times the [[solar luminosity]] from its [[stellar atmosphere|outer atmosphere]] at an [[effective temperature]] of 5,115&nbsp;K.<ref name=Rains2020/> Unusually for a star of this class, it shows a [[Photometry (astronomy)|photometric]] [[Variable star|variability]] of 0.04 in magnitude, which may be due to a previous mass transfer from the secondary companion, or else from an undiscovered third companion.<ref name=Fuhrmann2012/>


The companion is about 7 magnitudes fainter than the primary and may be the source of the [[X-ray astronomy|X
The companion is about 7 magnitudes fainter than the primary and may be the source of the [[X-ray astronomy|X
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==References==
==References==
{{reflist|refs=
{{reflist|refs=

<ref name=Rains2020>{{cite journal
| title=Precision angular diameters for 16 southern stars with VLTI/PIONIER
⚫
| display-authors=1 | last1=Rains | first1=Adam D.
⚫
| last2=Ireland | first2=Michael J. | last3=White | first3=Timothy R.
| last4=Casagrande | first4=Luca | last5=Karovicova | first5=I.
⚫
| journal=Monthly Notices of the Royal Astronomical Society
⚫
| volume=493 | issue=2 | pages=2377–2394 | date=April 2020
| arxiv=2004.02343 | bibcode=2020MNRAS.493.2377R
| doi=10.1093/mnras/staa282 }}</ref>


<ref name=vanLeeuwen2007>{{citation
<ref name=vanLeeuwen2007>{{citation
Line 90: Line 101:
| doi=10.1088/0067-0049/203/2/30 | bibcode=2012ApJS..203...30F
| doi=10.1088/0067-0049/203/2/30 | bibcode=2012ApJS..203...30F
| postscript=. }}</ref>
| postscript=. }}</ref>

<ref name=Mcdonald2012>{{citation
⚫
| display-authors=1 | last1=McDonald | first1=I.
⚫
| last2=Zijlstra | first2=A. A. | last3=Boyer | first3=M. L.
| title=Fundamental Parameters and Infrared Excesses of Hipparcos Stars
⚫
| journal=Monthly Notices of the Royal Astronomical Society
⚫
| volume=427 | issue=1 | pages=343–57 | date=2012
| bibcode=2012MNRAS.427..343M | arxiv=1208.2037
| doi = 10.1111/j.1365-2966.2012.21873.x | postscript=. }}</ref>


<ref name=Poveda1994>{{citation
<ref name=Poveda1994>{{citation
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[[Category:G-type subgiants]]
[[Category:G-type subgiants]]
⚫
[[Category:Binary stars]]
[[Category:Eridanus (constellation)]]
[[Category:Eridanus (constellation)]]
[[Category:Bayer objects|Eridani, Chi]]
[[Category:Bayer objects|Eridani, Chi]]
⚫
[[Category:Durchmusterung objects]]
⚫
[[Category:Gliese and GJ objects|0081]]
[[Category:Henry Draper Catalogue objects|011937]]
[[Category:Henry Draper Catalogue objects|011937]]
[[Category:Hipparcos objects|009007]]
[[Category:Hipparcos objects|009007]]
[[Category:HR objects|0566]]
[[Category:HR objects|0566]]
⚫
[[Category:Binary stars]]
⚫
[[Category:Gliese and GJ objects|0081]]
⚫
[[Category:Durchmusterung objects]]

Revision as of 04:17, 6 November 2020

χ Eridani
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Eridanus
Right ascension 01h 55m 57.47212s[1]
Declination −51° 36′ 32.0325″[1]
Apparent magnitude (V) 3.70[2] / 10.7[3]
Characteristics
Spectral type G8IV[4]
U−B color index +0.46[2]
B−V color index +0.85[2]
Astrometry
Proper motion (μ) RA: +680.92[1] mas/yr
Dec.: −283.46[1] mas/yr
Parallax (π)56.02 ± 0.38 mas[1]
Distance58.2 ± 0.4 ly
(17.9 ± 0.1 pc)
Absolute magnitude (MV)2.39 / 9.4[3]
Details[5]
A
Mass1.58[6] M☉
Radius3.993±0.027 R☉
Luminosity9.84±0.39 L☉
Surface gravity (log g)3.42±0.10 cgs
Temperature5,115±49 K
Metallicity [Fe/H]−0.18±0.07 dex
Rotational velocity (v sin i)4.50 km/s
Other designations
χ Eri, FK5 68, GJ 81, HD 11937, HIP 9007, HR 566, SAO 232573[7]
Database references
SIMBADdata
ARICNSA
B

χ Eridani (Latinised as Chi Eridani) is a binary star[8] system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.70.[2] The distance to this system, as determined using the parallax method, is around 58 light years.[1] The pair had an angular separation of 5.0 arcseconds as of 1994. This corresponds to a projected separation of around 128 AU.[3]

The primary component is an evolving G-type subgiant star with a stellar classification of G8 IV.[4] It is about 1.6 times the mass of the Sun and has 4 times the Sun's radius.[6] The star shines with 10 times the solar luminosity from its outer atmosphere at an effective temperature of 5,115 K.[5] Unusually for a star of this class, it shows a photometric variability of 0.04 in magnitude, which may be due to a previous mass transfer from the secondary companion, or else from an undiscovered third companion.[6]

The companion is about 7 magnitudes fainter than the primary and may be the source of the X -ray emission from this system. This emission has a luminosity of 504.4×1027 erg s−1.[6]

References

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b c Poveda, A.; et al. (April 1994), "Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems", Revista Mexicana de Astronomía y Astrofísica, 28 (1): 43–89, Bibcode:1994RMxAA..28...43P. See pp. 58–59.
  4. ^ a b Torres, C. A. O.; et al. (December 2006), "Search for associations containing young stars (SACY). I. Sample and searching method", Astronomy and Astrophysics, 460 (3): 695–708, arXiv:astro-ph/0609258, Bibcode:2006A&A...460..695T, doi:10.1051/0004-6361:20065602.
  5. ^ a b Rains, Adam D.; et al. (April 2020). "Precision angular diameters for 16 southern stars with VLTI/PIONIER". Monthly Notices of the Royal Astronomical Society. 493 (2): 2377–2394. arXiv:2004.02343. Bibcode:2020MNRAS.493.2377R. doi:10.1093/mnras/staa282.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  6. ^ a b c d Fuhrmann, K.; Chini, R. (2012), "Multiplicity among F-type Stars", The Astrophysical Journal Supplement, 203 (2): 20, Bibcode:2012ApJS..203...30F, doi:10.1088/0067-0049/203/2/30, 30.
  7. ^ "* chi Eri -- Pre-main sequence Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-27.{{cite web}}: CS1 maint: postscript (link)
  8. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.{{citation}}: CS1 maint: unflagged free DOI (link)
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