HD 102365: Difference between revisions

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{{Short description|Binary star system in the constellation Centaurus}}
{{Starbox begin
{{Starbox begin}}
| name=HR 4523 A/B }}
{{Starbox observe
{{Starbox observe 2s
| epoch=J2000
| epoch = J2000
⚫
| constell = [[Centaurus]]
⚫
| ra={{RA|11|46|31.07263}}<ref name=aaa474_2_653/>
| component1 = HD 102365 A
⚫
| dec={{DEC|−40|30|01.2722}}<ref name=aaa474_2_653/>
| appmag_v=4.88<ref name=ibsh8_30/>/15<ref name=rmaa28_1_43/>
| ra1 = {{RA|11|46|31.07253}}<ref name=GaiaDR3a/>
⚫
| dec1 = {{DEC|−40|30|01.2859}}<ref name=GaiaDR3a/>
⚫
| constell=[[Centaurus]] }}
| appmag_v1 = 4.88<ref name=ibsh8_30/>
| component2 = HD 102365 B
⚫
| ra2 = {{RA|11|46|32.68988}}<ref name=GaiaDR3b/>
| dec2 = {{DEC|−40|29|47.6048}}<ref name=GaiaDR3b/>
| appmag_v2 = 15<ref name=rmaa28_1_43/>
}}
{{Starbox character
{{Starbox character
| class=G2V<ref name=apj132_1_161/>/M4V<ref name=aphs190_1_1/>
| class = G2V<ref name=apj132_1_161/> + M4V<ref name=aphs190_1_1/>
| b-v=0.67<ref name=ibsh8_30/>
| b-v = 0.67<ref name=ibsh8_30/>
| u-b=0.10<ref name=ibsh8_30/>
| u-b = 0.10<ref name=ibsh8_30/>
| variable= }}
| variable =
}}
{{Starbox astrometry
{{Starbox astrometry
| component1 = HD 102365 A
| radial_v={{nowrap|15.3 ± 0.9}}<ref name=rgcrv/>
| prop_mo_ra=−1530.99<ref name=aaa474_2_653/>
| radial_v = {{val|16.94|0.12}}<ref name=GaiaDR3a/>
| prop_mo_ra = −1530.971
| prop_mo_dec=403.67<ref name=aaa474_2_653/>
| prop_mo_dec = +403.287
⚫
| parallax=108.45
| pm_footnote = <ref name=GaiaDR3a/>
⚫
| p_error=0.22
⚫
| parallax = 107.3024
⚫
| parallax_footnote=<ref name=aaa474_2_653/> }}
⚫
| p_error = 0.0873
⚫
| parallax_footnote = <ref name=GaiaDR3a/>
| absmag_v = 5.07<ref name=aaa501_3_941/>
| component2 = HD 102365 B
| radial_v2 = {{val|17.23|0.27}}<ref name=GaiaDR3b/>
| prop_mo_ra2 = −1534.679
| prop_mo_dec2 = +381.396
| pm_footnote2 = <ref name=GaiaDR3b/>
| parallax2 = 107.4237
| p_error2 = 0.0351
| parallax_footnote2 = <ref name=GaiaDR3b/>
| absmag_v2 =
}}
{{Starbox detail
{{Starbox detail
| component1 = A
| mass=0.889<ref name=apjss168_2_297/>
| radius=0.96<ref name=apjss168_2_297/>
| mass = 0.889<ref name=apjss168_2_297/>
| luminosity=0.85<ref name=ab6_2_308/>
| radius = 0.96<ref name=apjss168_2_297/>
| temperature=5,643<ref name=ab6_2_308/>
| luminosity = 0.85<ref name=ab6_2_308/>
| metal_fe=−0.28<ref name=ab6_2_308/>
| temperature = 5,643<ref name=ab6_2_308/>
| gravity=4.51<ref name=apj132_1_161/>
| metal_fe = −0.28<ref name=ab6_2_308/>
| rotational_velocity=0.5<ref name=aaa493_3_1099/>
| gravity = 4.51<ref name=apj132_1_161/>
| age_gyr=4.5–5.7<ref name=apj687_2_1264/>
| rotational_velocity = 0.5<ref name=aaa493_3_1099/>
| age_gyr = 4.5–5.7<ref name=apj687_2_1264/>
}}
}}
{{Starbox catalog
{{Starbox catalog
| names=66 [[Gould designation|G.]] Centauri, [[Gliese-Jahreiss catalogue|GJ]]&nbsp;442, [[Harvard Revised catalogue|HR]]&nbsp;4523, [[Cordoba Durchmusterung|CD]]&nbsp;-39&deg;7301, [[Henry Draper catalogue|HD]]&nbsp;102365, [[Luyten Half-Second catalogue|LHS]]&nbsp;311, [[Luyten Two-Tenths catalogue|LTT]]&nbsp;4373, [[General Catalogue of Trigonometric Parallaxes|GCTP]]&nbsp;2725.00, [[Smithsonian Astrophysical Observatory|SAO]]&nbsp;223020, [[Hipparcos catalogue|HIP]]&nbsp;57443.<ref name=SIMBAD/> }}
| names = {{odlist | G=66 Centauri | GJ=442 | HR=4523 | CD=−39°7301 | HD=102365 | LHS=311 | LTT=4373 | GCTP=2725.00 | SAO=223020 | HIP=57443 }}<ref name=SIMBAD/>
}}
{{Starbox reference
{{Starbox reference
| Simbad=LHS+311
| Simbad=LHS+311
| sn=A
⚫
| ARICNS=00904 }}
| Simbad2=GJ+442+B
| sn2=B
⚫
| ARICNS=00904
}}
{{Starbox end}}
{{Starbox end}}
⚫
'''HR 4523''' ('''66 G. Centauri''') is a [[binary star]] system that is located in the [[constellation]] of [[Centaurus]]. The larger member of the system is a G-type star that is smaller than the [[Sun]] but of similar mass. It has a common proper motion companion that was discovered by [[Willem Jacob Luyten|W. J. Luyten]] in 1960.<ref name=aphs190_1_1/> This [[red dwarf|M-type star]] appears to be in a wide orbit around the primary at a current separation of about 211 Astronomical Units (A.U.),<ref name=aphs190_1_1/> (or 211 times the separation of the Earth from the Sun). By comparison, Neptune orbits at an average distance of 30 A.U.


⚫
'''HD 102365''' ('''66 G. Centauri''') is a [[binary star]] system that is located in the northeastern part of the [[Centaurus]] [[constellation]], at a distance of about {{Convert|30.4|ly|pc|lk=on|abbr=off}} from the [[Solar System]]. The larger member of the system is a G-type star that is smaller than the [[Sun]] but of similar mass. It has a [[common proper motion]] companion that was discovered by [[Willem Jacob Luyten|W. J. Luyten]] in 1960.<ref name=aphs190_1_1/> This M-type star appears to be in a wide orbit around the primary at a current separation of about 211 [[astronomical unit]]s (AU),<ref name=aphs190_1_1/> (or 211 times the separation of the Earth from the Sun). By comparison, [[Neptune]] orbits at an average distance of 30 AU.
⚫
The primary star in this system has an estimated 86%<ref name=apj701_2_1732/> to 89% the [[Solar mass|mass of the Sun]], 96% of the [[Solar radius|Sun's radius]],<ref name=apjss168_2_297/> and 85% of the [[Solar luminosity|Sun's luminosity]].<ref name=ab6_2_308/> Age estimates range from 4.5–5.7&nbsp;Gyr<ref name=apj687_2_1264/> up to 7.1&nbsp;Gyr<ref name=aaa501_3_941/> or 9.48&nbsp;Gyr.<ref name=apjss168_2_297/> Compared to the Sun, it only has about 52%<ref name=metal/> of the abundance of elements other than hydrogen and helium; what astronomers term the [[metallicity]] of a star.

== Description ==
⚫
The [[stellar classification]] for the primary star in this system is G2V;<ref name=apj132_1_161/> the same as the Sun. That of the [[red dwarf]] companion is M4V.<ref name=aphs190_1_1/> The primary star has an estimated 86%<ref name=apj701_2_1732/> to 89% the [[Solar mass|mass of the Sun]], 96% of the [[Solar radius|Sun's radius]],<ref name=apjss168_2_297/> and 85% of the [[Solar luminosity|Sun's luminosity]].<ref name=ab6_2_308/> It is a slow rotator, with a [[stellar rotation|projected rotational velocity]] of 0.5&nbsp;km/s.<ref name=aaa493_3_1099/> Age estimates range from 4.5 to 5.7&nbsp;billion years (Gyr)<ref name=apj687_2_1264/> up to 7.1&nbsp;Gyr<ref name=aaa501_3_941/> or 9.48&nbsp;Gyr.<ref name=apjss168_2_297/> Compared to the Sun, it only has about 52%<ref name=metal/> of the abundance of elements other than hydrogen and helium; what astronomers term the [[metallicity]] of a star.


The HR 4523 system is a member of the [[Epsilon Indi]] [[Stellar association|Moving Group]], although it is most likely an interloper. (The star is older and has a different composition than the other group members.)<ref name=aaa68_1_27/> It has [[space velocity]] components {{nowrap|[''U'', ''V'', ''W'']}} = {{nowrap|[−67, −40, +4] km/s}}.<ref name=gliese1969/>
This star system has a relatively large proper motion.<ref name=SIMBAD/> The HR 4523 system is presently located within the [[Epsilon Indi Moving Group]], although it gives itself away as an interloper, since the star is older and has a different composition than the group members.<ref name=aaa68_1_27/> It has [[space velocity (astronomy)|space velocity]] components {{nowrap|[''U'', ''V'', ''W'']}} = {{nowrap|[−67, −40, +4] km/s}}.<ref name=gliese1969/>


== Planetary system ==
== Planetary system ==


The primary star is believed to be orbited by a Neptune-like planet with a mass 16 times that of the Earth. The orbital period of this planet is 122.1 days. No other planets have been discovered orbiting this star.<ref name=apj727_103/>
The primary star is believed to be orbited by a Neptune-like planet with a [[minimum mass]] 16 times that of the Earth. The orbital period of this planet is 122.1 days. No other planets have been discovered orbiting this star.<ref name=apj727_103/> While a 2013 study was unable to confirm this planet,<ref name="Zechmeister2013"/> it was confirmed by a 2023 study, with updated parameters.<ref name="Laliotis2023"/>{{rp|27}}


An examination of this system in the [[infrared]] did not reveal an [[infrared excess|excess emission]] that would otherwise suggest the presence of a circumstellar [[debris disk]].<ref name=apj652_2_1674/>
{{OrbitboxPlanet begin|table_ref=<ref name=epe_HD_102365b/>}}

{{OrbitboxPlanet begin
| table_ref = <ref name=apj727_103/><ref name="Laliotis2023"/>
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = [[HD 102365 b|b]]
| exoplanet = b
| mass = {{nowrap|0.05 ± 0.008}}
| mass_earth = {{val|9.34|1.52|1.5|p=≥}}
| period = {{nowrap|122.1 ± 0.3}}
| period = {{val|121.3|0.25}}
| semimajor = {{nowrap|0.46 ± 0.04}}
| semimajor = {{val|0.46|0.04}}
| eccentricity = {{nowrap|0.34 ± 0.14}}
| eccentricity = {{val|0.28|0.15}}
}}
}}
{{Orbitbox end}}
{{Orbitbox end}}

==In popular culture==
The [[couch gag]] for ''[[Bart's Not Dead]]'' in the television series ''[[The Simpsons]]'' has an alien family sitting on a couch in this star system. The adult male alien asks why [[Homer J. Simpson|Homer]] sounds like [[Walter Matthau]].


==References==
==References==
{{reflist|refs=
{{reflist|refs=


<ref name=GaiaDR3a>{{Cite Gaia DR3|5381537023379295232}}</ref>
<ref name=aaa474_2_653>{{citation | last1=van Leeuwen | first1=F. | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | month=November | year=2007 | pages=653–664 | doi=10.1051/0004-6361:20078357 | bibcode=2007A&A...474..653V | arXiv=0708.1752 }}</ref>
<ref name=GaiaDR3b>{{Cite Gaia DR3|5381537023379295744}}</ref>


<ref name=ibsh8_30>{{citation | last1=Feinstein | first1=A. | title=Photoelectric observations of Southern late-type stars | journal=The Information Bulletin for the Southern Hemisphere | volume=8 | page=30 | year=1966 | bibcode=1966IBSH....8...30F }}</ref>
<ref name=ibsh8_30>{{citation | last1=Feinstein | first1=A. | title=Photoelectric observations of Southern late-type stars | journal=The Information Bulletin for the Southern Hemisphere | volume=8 | page=30 | year=1966 | bibcode=1966IBSH....8...30F }}</ref>


<ref name=apj132_1_161>{{citation | display-authors=1 | last1=Gray | first1=R. O. | last2=Corbally | first2=C. J. | last3=Garrison | first3=R. F. | last4=McFadden | first4=M. T. | last5=Bubar | first5=E. J. | last6=McGahee | first6=C. E. | last7=O'Donoghue | first7=A. A. | last8=Knox | first8=E. R. | title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample | journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170 | month=July | year=2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G }}</ref>
<ref name=apj132_1_161>{{citation | display-authors=1 | last1=Gray | first1=R. O. | last2=Corbally | first2=C. J. | last3=Garrison | first3=R. F. | last4=McFadden | first4=M. T. | last5=Bubar | first5=E. J. | last6=McGahee | first6=C. E. | last7=O'Donoghue | first7=A. A. | last8=Knox | first8=E. R. | title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample | journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170 |date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G |arxiv = astro-ph/0603770 | s2cid=119476992 }}</ref>


<ref name=aphs190_1_1>{{citation | display-authors=1 | last1=Raghavan | first1=Deepak | last2=McAlister | first2=Harold A. | last3=Henry | first3=Todd J. | last4=Latham | first4=David W. | last5=Marcy | first5=Geoffrey W. | last6=Mason | first6=Brian D. | last7=Gies | first7=Douglas R. | last8=White | first8=Russel J. | last9=ten Brummelaar | first9=Theo A. | title=A Survey of Stellar Families: Multiplicity of Solar-type Stars | journal=The Astrophysical Journal Supplement | volume=190 | issue=1 | pages=1-42 | month=September | year=2010 | doi=10.1088/0067-0049/190/1/1 | bibcode=2010ApJS..190....1R }} For the adopted physical separation, see Table 11 in the appendix.</ref>
<ref name=aphs190_1_1>{{citation | display-authors=1 | last1=Raghavan | first1=Deepak | last2=McAlister | first2=Harold A. | last3=Henry | first3=Todd J. | last4=Latham | first4=David W. | last5=Marcy | first5=Geoffrey W. | last6=Mason | first6=Brian D. | last7=Gies | first7=Douglas R. | last8=White | first8=Russel J. | last9=ten Brummelaar | first9=Theo A. | title=A Survey of Stellar Families: Multiplicity of Solar-type Stars | journal=The Astrophysical Journal Supplement | volume=190 | issue=1 | pages=1–42 |date=September 2010 | doi=10.1088/0067-0049/190/1/1 | bibcode=2010ApJS..190....1R |arxiv = 1007.0414 | s2cid=368553 }} For the adopted physical separation, see Table 11 in the appendix.</ref>


⚫
<ref name=apj701_2_1732>{{citation | display-authors=1 | title=The Frequency of Low-Mass Exoplanets | last1=O'Toole | first1=S. J. | last2=Jones | first2=H. R. A. | last3=Tinney | first3=C. G. | last4=Butler | first4=R. P. | last5=Marcy | first5=G. W. | last6=Carter | first6=B. | last7=Bailey | first7=J. | last8=Wittenmyer | first8=R. A. | journal=The Astrophysical Journal | volume=701 | issue=2 | pages=1732–1741 |date=August 2009 | doi=10.1088/0004-637X/701/2/1732 | bibcode=2009ApJ...701.1732O |arxiv = 0906.4619 | s2cid=18041021 }}</ref>
<ref name=rgcrv>{{citation | first1=D. S. | last1=Evans | contribution= The Revision of the General Catalogue of Radial Velocities | title=Proceedings from IAU Symposium no. 30 | page=57 | publisher=Academic Press | date=June 20–24, 1966 |location=London, England | bibcode=1967IAUS...30...57E }}</ref>


<ref name=apj701_2_1732>{{citation | display-authors=1 | title=The Frequency of Low-Mass Exoplanets | last1=O'Toole | first1=S. J. | last2=Jones | first2=H. R. A. | last3=Tinney | first3=C. G. | last4=Butler | first4=R. P. | last5=Marcy | first5=G. W. | last6=Carter | first6=B. | last7=Bailey | first7=J. | last8=Wittenmyer | first8=R. A. | journal=The Astrophysical Journal | volume=701 | issue=2 | pages=1732-1741 | month=August | year=2009 | doi=10.1088/0004-637X/701/2/1732 | bibcode=2009ApJ...701.1732O }}</ref>
<ref name=apjss168_2_297>{{citation | display-authors=1 | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6=Jeff A. | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | journal=The Astrophysical Journal Supplement Series | volume=168 | issue=2 | pages=297–318 |date=February 2007 | doi=10.1086/509763 | bibcode=2007ApJS..168..297T |arxiv = astro-ph/0607235 | s2cid=18775378 }}</ref>

⚫
<ref name=apjss168_2_297>{{citation | display-authors=1 | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6=Jeff A. | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | journal=The Astrophysical Journal Supplement Series | volume=168 | issue=2 | pages=297-318 | month=February | year=2007 | doi=10.1086/509763 | bibcode=2007ApJS..168..297T }}</ref>


<ref name=aaa68_1_27>{{citation | last1=Kovacs | first1=N. | last2=Foy | first2=R. | title=A detailed analysis of three stars in the Eggen's Epsilon INDI moving group | journal=Astronomy and Astrophysics | year=1978 | volume=68 | issue=1–2 | pages=27–31 | bibcode=1978A&A....68...27K }}</ref>
<ref name=aaa68_1_27>{{citation | last1=Kovacs | first1=N. | last2=Foy | first2=R. | title=A detailed analysis of three stars in the Eggen's Epsilon INDI moving group | journal=Astronomy and Astrophysics | year=1978 | volume=68 | issue=1–2 | pages=27–31 | bibcode=1978A&A....68...27K }}</ref>


<ref name=ab6_2_308>{{citation | last1=Porto de Mello | first1=G. | last2=del Peloso | first2=E. F. | last3=Ghezzi | first3=L. | title=Astrobiologically Interesting Stars Within 10 Parsecs of the Sun | journal=Astrobiology | year=2006 | volume=6 | issue=2 | pages=308–331 | bibcode=2006AsBio...6..308P | doi=10.1089/ast.2006.6.308 | pmid=16689649 |arxiv = astro-ph/0511180 }}</ref>
<ref name=ab6_2_308>{{citation | last1=Porto de Mello | first1=G. | last2=del Peloso | first2=E. F. | last3=Ghezzi | first3=L. | title=Astrobiologically Interesting Stars Within 10 Parsecs of the Sun | journal=Astrobiology | year=2006 | volume=6 | issue=2 | pages=308–331 | bibcode=2006AsBio...6..308P | doi=10.1089/ast.2006.6.308 | pmid=16689649 |arxiv = astro-ph/0511180 | s2cid=119459291 }}</ref>
<ref name=aaa493_3_1099>{{citation | last1=Schröder | first1=C. | last2=Reiners | first2=A. | last3=Schmitt | first3=J. H. M. M. | title=Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo | journal=Astronomy and Astrophysics | volume=493 | issue=3 | pages=1099–1107 | month=January | year=2009 | doi=10.1051/0004-6361:200810377 | bibcode=2009A&A...493.1099S }}</ref>
<ref name=aaa493_3_1099>{{citation | last1=Schröder | first1=C. | last2=Reiners | first2=Ansgar | last3=Schmitt | first3=Jürgen H. M. M. | title=Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo | journal=Astronomy and Astrophysics | volume=493 | issue=3 | pages=1099–1107 | date=January 2009 | doi=10.1051/0004-6361:200810377 | bibcode=2009A&A...493.1099S | doi-access=free | url=http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9690/aa10377-08.pdf?sequence=2 }}{{Dead link|date=September 2023 |bot=InternetArchiveBot |fix-attempted=yes }}</ref>


<ref name=apj687_2_1264>{{citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 | month=November | year=2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M }}</ref>
<ref name=apj687_2_1264>{{citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 |date=November 2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M |arxiv = 0807.1686 | s2cid=27151456 }}</ref>


<ref name=SIMBAD>{{citation | title=LHS 311 -- High proper-motion Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=LHS+311 | accessdate=2011-10-11 }}</ref>
<ref name=SIMBAD>{{cite simbad | title=HD 102365 | access-date=2011-10-11 }}</ref>


<ref name=aaa501_3_941>{{citation | last1=Holmberg | first1=J. | last2=Nordström | first2=B. | last3=Andersen | first3=J. | title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics | journal=Astronomy and Astrophysics | volume=501 | issue=3 | pages=941-947 | month=July | year=2009 | doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H }}</ref>
<ref name=aaa501_3_941>{{citation | last1=Holmberg | first1=J. | last2=Nordström | first2=B. | last3=Andersen | first3=J. | title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics | journal=Astronomy and Astrophysics | volume=501 | issue=3 | pages=941–947 |date=July 2009 | doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H |arxiv = 0811.3982 | s2cid=118577511 }}</ref>


<ref name=metal>For a metallicity of [Fe/H] = −0.28 dex, the proportion of metals is given by 10<sup>−0.28</sup>, or 52%.</ref>
<ref name=metal>For a metallicity of [Fe/H] = −0.28 dex, the proportion of metals is given by 10<sup>−0.28</sup>, or 52%.</ref>


<ref name=rmaa28_1_43>{{citation | display-authors=1 | last1=Poveda | first1=A. | last2=Herrera | first2=M. A. | last3=Allen | first3=C. | last4=Cordero | first4=G. | last5=Lavalley | first5=C. | title=Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems | journal=Revista Mexicana de Astronomía y Astrofísica | volume=28 | issue=1 | pages=43-89 | month=April | year=1994 | bibcode=1994RMxAA..28...43P }}</ref>
<ref name=rmaa28_1_43>{{citation | display-authors=1 | last1=Poveda | first1=A. | last2=Herrera | first2=M. A. | last3=Allen | first3=C. | last4=Cordero | first4=G. | last5=Lavalley | first5=C. | title=Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems | journal=Revista Mexicana de Astronomía y Astrofísica | volume=28 | issue=1 | pages=43–89 |date=April 1994 | bibcode=1994RMxAA..28...43P }}</ref>


<ref name=gliese1969>{{citation | last1=Gliese | first1=W. | contribution=Catalogue of Nearby Stars. Edition 1969 | title=Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg | issue=22 | location=Karlsruhe | year=1969 | bibcode=1969VeARI..22....1G }}</ref>
<ref name=gliese1969>{{citation | last1=Gliese | first1=W. | contribution=Catalogue of Nearby Stars. Edition 1969 | title=Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg | issue=22 | location=Karlsruhe | year=1969 | volume=22 | page=1 | bibcode=1969VeARI..22....1G }}</ref>


<ref name=apj727_103>{{citation | display-authors=1 | last1=Tinney | first1=C. G. | last2=Butler | first2=R. Paul | last3=Jones | first3=Hugh R. A. | last4=Wittenmyer | first4=Robert A. | last5=O'Toole | first5=Simon | last6=Bailey | first6=Jeremy | last7=Carter | first7=Brad D. | title=The Anglo-Australian Planet Search. XX. A Solitary Ice-giant Planet Orbiting HD 102365 | journal=The Astrophysical Journal | year=2011 | volume=727 | issue=2 | page=103 | doi=10.1088/0004-637X/727/2/103 | bibcode=2011ApJ...727..103T }}</ref>
<ref name=apj727_103>{{citation | display-authors=1 | last1=Tinney | first1=C. G. | last2=Butler | first2=R. Paul | last3=Jones | first3=Hugh R. A. | last4=Wittenmyer | first4=Robert A. | last5=O'Toole | first5=Simon | last6=Bailey | first6=Jeremy | last7=Carter | first7=Brad D. | title=The Anglo-Australian Planet Search. XX. A Solitary Ice-giant Planet Orbiting HD 102365 | journal=The Astrophysical Journal | year=2011 | volume=727 | issue=2 | page=103 | doi=10.1088/0004-637X/727/2/103 | bibcode=2011ApJ...727..103T | s2cid=54984338 | url=http://eprints.usq.edu.au/20483/3/Tinney_Butler_Jones_etal_AJ_2011_SV.pdf }}</ref>


<ref name=apj652_2_1674>{{citation | display-authors=1 | last1=Beichman | first1=C. A. | last2=Bryden | first2=G. | last3=Stapelfeldt | first3=K. R. | last4=Gautier | first4=T. N. | last5=Grogan | first5=K. | last6=Shao | first6=M. | last7=Velusamy | first7=T. | last8=Lawler | first8=S. M. | last9=Blaylock | first9=M. | title=New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets | journal=The Astrophysical Journal | volume=652 | issue=2 | pages=1674–1693 |date=December 2006 | doi=10.1086/508449 | bibcode=2006ApJ...652.1674B |arxiv = astro-ph/0611682 | s2cid=14207148 }}</ref>
<ref name=epe_HD_102365b>{{citation | first1=Jean | last1=Schneider | contribution=Planet : HD 102365 b | title=Extrasolar Planets Encyclopaedia | url=http://exoplanet.eu/planet.php?p1=HD+102365&p2=b | accessdate=2011-10-11 }}</ref>

<ref name="Zechmeister2013">{{cite journal |last1=Zechmeister |first1=M. |last2=Kürster |first2=M. |display-authors=etal |date=April 2013 |title=The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars |journal=[[Astronomy & Astrophysics]] |volume=552 |issue= |pages=A78 |doi=10.1051/0004-6361/201116551 |arxiv=1211.7263 |bibcode=2013A&A...552A..78Z|s2cid=53694238 }}</ref>

<ref name="Laliotis2023">{{cite journal |last1=Laliotis |first1=Katherine |last2=Burt |first2=Jennifer A. |display-authors=etal |date=February 2023 |title=Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions |journal=[[The Astronomical Journal]] |volume= 165|issue= 4|page=176 |doi= 10.3847/1538-3881/acc067|arxiv=2302.10310 |bibcode=2023AJ....165..176L |doi-access=free }}</ref>


}}
}}


==External links==
==External links==
* {{citation | title=HR 4523 AB | publisher=SolStation | url=http://www.solstation.com/stars/hr4523ab.htm | accessdate=2011-10-11 }}
* {{citation | title=HR 4523 AB | publisher=SolStation | url=http://www.solstation.com/stars/hr4523ab.htm | access-date=2011-10-11 }}


{{Nearest star systems|7}}
{{Stars of Centaurus}}
<!-- Properties -->
{{Nearest bright star systems|4.}}
{{DEFAULTSORT:HD 102365}}
⚫
[[Category:Centaurus constellation]]
[[Category:G-type main sequence stars]]
[[Category:G-type main-sequence stars]]
[[Category:Solar analogs|HR, 4523]]
⚫
[[Category:Planetary systems with one confirmed planet]]
[[Category:M-type main-sequence stars]]
[[Category:Binary stars]]
<!-- Catalogues -->
⚫
[[Category:Centaurus]]
[[Category:Durchmusterung objects|CD-39 07301]]
[[Category:Gliese and GJ objects|0442]]
[[Category:Gould objects|Centauri, 66]]
[[Category:Henry Draper Catalogue objects|102365]]
[[Category:Henry Draper Catalogue objects|102365]]
[[Category:HIP objects|57433]]
[[Category:Hipparcos objects|057433]]
[[Category:HR objects|4523]]
[[Category:Bright Star Catalogue objects|4523]]
⚫
[[Category:Planetary systems]]

[[es:HR 4523]]
[[fa:اچ‌آر ۴۵۲۳]]
[[fr:HR 4523]]
[[ko:HR 4523]]
[[id:HR 4523]]
[[ru:HR 4523]]
[[sk:HR 4523]]

Latest revision as of 02:19, 6 May 2024

HD 102365
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
HD 102365 A
Right ascension 11h 46m 31.07253s[1]
Declination −40° 30′ 01.2859″[1]
Apparent magnitude (V) 4.88[2]
HD 102365 B
Right ascension 11h 46m 32.68988s[3]
Declination −40° 29′ 47.6048″[3]
Apparent magnitude (V) 15[4]
Characteristics
Spectral type G2V[5] + M4V[6]
U−B color index 0.10[2]
B−V color index 0.67[2]
Astrometry
HD 102365 A
Radial velocity (Rv)16.94±0.12[1] km/s
Proper motion (μ) RA: −1530.971 mas/yr[1]
Dec.: +403.287 mas/yr[1]
Parallax (π)107.3024 ± 0.0873 mas[1]
Distance30.40 ± 0.02 ly
(9.319 ± 0.008 pc)
Absolute magnitude (MV)5.07[7]
HD 102365 B
Radial velocity (Rv)17.23±0.27[3] km/s
Proper motion (μ) RA: −1534.679 mas/yr[3]
Dec.: +381.396 mas/yr[3]
Parallax (π)107.4237 ± 0.0351 mas[3]
Distance30.362 ± 0.010 ly
(9.309 ± 0.003 pc)
Details
A
Mass0.889[8] M☉
Radius0.96[8] R☉
Luminosity0.85[9] L☉
Surface gravity (log g)4.51[5] cgs
Temperature5,643[9] K
Metallicity [Fe/H]−0.28[9] dex
Rotational velocity (v sin i)0.5[10] km/s
Age4.5–5.7[11] Gyr
Other designations
CD−39°7301, GJ 442, HD 102365, HIP 57443, HR 4523, SAO 223020, G 66 Centauri, LHS 311, LTT 4373[12]
Database references
SIMBADA
B
ARICNSdata

HD 102365 (66 G. Centauri) is a binary star system that is located in the northeastern part of the Centaurus constellation, at a distance of about 30.4 light-years (9.3 parsecs) from the Solar System. The larger member of the system is a G-type star that is smaller than the Sun but of similar mass. It has a common proper motion companion that was discovered by W. J. Luyten in 1960.[6] This M-type star appears to be in a wide orbit around the primary at a current separation of about 211 astronomical units (AU),[6] (or 211 times the separation of the Earth from the Sun). By comparison, Neptune orbits at an average distance of 30 AU.

Description[edit]

The stellar classification for the primary star in this system is G2V;[5] the same as the Sun. That of the red dwarf companion is M4V.[6] The primary star has an estimated 86%[13] to 89% the mass of the Sun, 96% of the Sun's radius,[8] and 85% of the Sun's luminosity.[9] It is a slow rotator, with a projected rotational velocity of 0.5 km/s.[10] Age estimates range from 4.5 to 5.7 billion years (Gyr)[11] up to 7.1 Gyr[7] or 9.48 Gyr.[8] Compared to the Sun, it only has about 52%[14] of the abundance of elements other than hydrogen and helium; what astronomers term the metallicity of a star.

This star system has a relatively large proper motion.[12] The HR 4523 system is presently located within the Epsilon Indi Moving Group, although it gives itself away as an interloper, since the star is older and has a different composition than the group members.[15] It has space velocity components [U, V, W] = [−67, −40, +4] km/s.[16]

Planetary system[edit]

The primary star is believed to be orbited by a Neptune-like planet with a minimum mass 16 times that of the Earth. The orbital period of this planet is 122.1 days. No other planets have been discovered orbiting this star.[17] While a 2013 study was unable to confirm this planet,[18] it was confirmed by a 2023 study, with updated parameters.[19]: 27 

An examination of this system in the infrared did not reveal an excess emission that would otherwise suggest the presence of a circumstellar debris disk.[20]

The HD 102365 planetary system[17][19]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥9.34+1.52
−1.5 M🜨 		0.46±0.04 121.3±0.25 0.28±0.15 — —

In popular culture[edit]

The couch gag for Bart's Not Dead in the television series The Simpsons has an alien family sitting on a couch in this star system. The adult male alien asks why Homer sounds like Walter Matthau.

References[edit]

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c Feinstein, A. (1966), "Photoelectric observations of Southern late-type stars", The Information Bulletin for the Southern Hemisphere, 8: 30, Bibcode:1966IBSH....8...30F
  3. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  4. ^ 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
  5. ^ a b c Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992
  6. ^ a b c d Raghavan, Deepak; et al. (September 2010), "A Survey of Stellar Families: Multiplicity of Solar-type Stars", The Astrophysical Journal Supplement, 190 (1): 1–42, arXiv:1007.0414, Bibcode:2010ApJS..190....1R, doi:10.1088/0067-0049/190/1/1, S2CID 368553 For the adopted physical separation, see Table 11 in the appendix.
  7. ^ a b Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511
  8. ^ a b c d Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763, S2CID 18775378
  9. ^ a b c d Porto de Mello, G.; del Peloso, E. F.; Ghezzi, L. (2006), "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun", Astrobiology, 6 (2): 308–331, arXiv:astro-ph/0511180, Bibcode:2006AsBio...6..308P, doi:10.1089/ast.2006.6.308, PMID 16689649, S2CID 119459291
  10. ^ a b Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377[permanent dead link]
  11. ^ a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID 27151456
  12. ^ a b "HD 102365". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2011-10-11.
  13. ^ O'Toole, S. J.; et al. (August 2009), "The Frequency of Low-Mass Exoplanets", The Astrophysical Journal, 701 (2): 1732–1741, arXiv:0906.4619, Bibcode:2009ApJ...701.1732O, doi:10.1088/0004-637X/701/2/1732, S2CID 18041021
  14. ^ For a metallicity of [Fe/H] = −0.28 dex, the proportion of metals is given by 10−0.28, or 52%.
  15. ^ Kovacs, N.; Foy, R. (1978), "A detailed analysis of three stars in the Eggen's Epsilon INDI moving group", Astronomy and Astrophysics, 68 (1–2): 27–31, Bibcode:1978A&A....68...27K
  16. ^ Gliese, W. (1969), "Catalogue of Nearby Stars. Edition 1969", Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg, vol. 22, Karlsruhe, p. 1, Bibcode:1969VeARI..22....1G{{citation}}: CS1 maint: location missing publisher (link)
  17. ^ a b Tinney, C. G.; et al. (2011), "The Anglo-Australian Planet Search. XX. A Solitary Ice-giant Planet Orbiting HD 102365" (PDF), The Astrophysical Journal, 727 (2): 103, Bibcode:2011ApJ...727..103T, doi:10.1088/0004-637X/727/2/103, S2CID 54984338
  18. ^ Zechmeister, M.; Kürster, M.; et al. (April 2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics. 552: A78. arXiv:1211.7263. Bibcode:2013A&A...552A..78Z. doi:10.1051/0004-6361/201116551. S2CID 53694238.
  19. ^ a b Laliotis, Katherine; Burt, Jennifer A.; et al. (February 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal. 165 (4): 176. arXiv:2302.10310. Bibcode:2023AJ....165..176L. doi:10.3847/1538-3881/acc067.
  20. ^ Beichman, C. A.; et al. (December 2006), "New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets", The Astrophysical Journal, 652 (2): 1674–1693, arXiv:astro-ph/0611682, Bibcode:2006ApJ...652.1674B, doi:10.1086/508449, S2CID 14207148

External links[edit]

Retrieved from "https://en.wikipedia.org/w/index.php?title=HD_102365&oldid=1222458888"