HD 117207
{{Short description|Star in the constellation Centaurus}}
{{Starbox begin}}
{{Starbox observe
| epoch = J2000
| constell = Centaurus
| dec = {{DEC|−35|34|15.5880}}
}}
{{Starbox character
| type =
| u-b =
| variable =
}}
{{Starbox astrometry
| radial_v = {{Val|−17.43|0.09}}
| prop_mo_ra = {{val|−205.904}}
| prop_mo_dec = {{val|−71.402}}
| parallax = 30.9440
| p_error = 0.0256
}}
{{Starbox detail
| mass = {{Val|1.053|0.028}}
| radius = {{Val|1.074|0.041}}
| luminosity = {{Val|1.163|0.002|0.003}}
| gravity = {{Val|4.371|0.039}}
| temperature = {{Val|5732|53|fmt=commas}}
| metal_fe = {{Val|0.19|0.03}}
| rotational_velocity =
| age_gyr = {{Val|4.192|2.274}}
}}
{{Starbox catalog
| names = {{odlist | CPD=−34°8913 | HD=117207 | HIP=65808 | SAO=204517 }}
}}
{{Starbox reference
| Simbad = HD+117207
| EPE = HD+117207
}}
{{End}}
HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24, it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of {{convert|105.4|ly|pc|lk=on|abbr=off}} from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s. It has an absolute magnitude of 4.67.
This object has a stellar classification of G7IV-V, showing blended spectral traits of a G-type main-sequence star and an older, evolving subgiant star. It is around four billion years old with 5% greater mass than the Sun and a 7% larger radius. The star is radiating 1.16 times the luminosity of the Sun from its photosphere at an effective temperature of 5,644 K.
In 2005, a planet was found orbiting the star using the radial velocity method, and was designated HD 117207 b. The orbital elements of this planet were refined in 2018, showing an orbital period of {{Convert|2621.75|days|years|2|disp=out|abbr=off}}, a semimajor axis of {{Val|3.79|ul=AU}}, and an eccentricity of 0.16. The minimum mass of this object is nearly double that of Jupiter. If an inner planet is orbiting the star, it must have an orbital period no greater than {{Convert|1263.5|days|years|2|disp=out|abbr=off}} to satisfy Hill's criteria for dynamic stability. In 2023, the inclination and true mass of HD 117207 b were determined via astrometry.
{{OrbitboxPlanet begin
| period_unit = year
}}
{{OrbitboxPlanet
| exoplanet = b
| mass = {{val|2.106|0.16|0.089}}
| period = {{val|7.136|0.034|0.035}}
| semimajor = {{val|3.773|0.036|0.035}}
| eccentricity = {{val|0.04|0.026|0.024}}
| inclination = {{val|76.6|9.3|12.0}} or {{val|103.4|12.0|9.3}}
}}
{{Orbitbox end}}
See also
References
{{Reflist|refs=
{{Cite Gaia DR2|6166183842771027328}}
{{Cite Gaia DR3|6166183842771027328}}
{{cite simbad | title=HD 117207 | access-date=2018-07-23}}
| 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 }}
| title=Abundances in the Local Region. III. Southern F, G, and K Dwarfs
| last1=Luck | first1=R. Earle
| journal=The Astronomical Journal
| volume=155 | issue=3 | id=111 | pages=31 | date=March 2018
| doi=10.3847/1538-3881/aaa9b5 | bibcode=2018AJ....155..111L | s2cid=125765376 | doi-access=free }}
| display-authors=1 | last1=Gray | first1=R. O.
| first2=C. J. | last2=Corbally | first3=R. F. | last3=Garrison
| first4=M. T. | last4=McFadden | first5=P. E. | last5=Robinson
| title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I
| 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 }}
| title=Exploring the realm of scaled solar system analogues with HARPS
| display-authors=1 | last1=Barbato | first1=D.
| last2=Sozzetti | first2=A. | last3=Desidera | first3=S.
| last4=Damasso | first4=M. | last5=Bonomo | first5=A. S.
| last6=Giacobbe | first6=P. | last7=Colombo | first7=L. S.
| last8=Lazzoni | first8=C. | last9=Claudi | first9=R.
| last10=Gratton | first10=R. | last11=LoCurto | first11=G.
| last12=Marzari | first12=F. | last13=Mordasini | first13=C.
| journal=Astronomy & Astrophysics
| volume=615 | id=A175 | pages=21 | date=August 2018
| doi=10.1051/0004-6361/201832791 | arxiv=1804.08329
| bibcode=2018A&A...615A.175B | s2cid=119099721 }}
| title=Catalog of Nearby Exoplanets
| last1=Butler | first1=R. P. | last2=Wright | first2=J. T.
| last3=Marcy | first3=G. W. | last4=Fischer | first4=D. A.
| last5=Vogt | first5=S. S. | last6=Tinney | first6=C. G.
| last7=Jones | first7=H. R. A. | last8=Carter | first8=B. D.
| last9=Johnson | first9=J. A. | display-authors=1
| journal=The Astrophysical Journal
| volume=646 | issue=1 | pages=505–522 | year=2006
| arxiv=astro-ph/0607493 | bibcode=2006ApJ...646..505B
| doi=10.1086/504701 | s2cid=119067572 }}
| title=Five New Extrasolar Planets
| last1=Marcy | first1=Geoffrey W. | last2=Butler | first2=R. Paul
| last3=Vogt | first3=Steven S. | last4=Fischer | first4=Debra A.
| last5=Henry | first5=Gregory W. | last6=Laughlin | first6=Greg
| last7=Wright | first7=Jason T. | last8=Johnson | first8=John A.
| display-authors=1 | journal=The Astrophysical Journal
| volume=619 | issue=1 | pages=570–584 | year=2005
| bibcode=2005ApJ...619..570M | doi=10.1086/426384
| citeseerx=10.1.1.516.6667 | s2cid=5803173 }}
{{cite journal |last1=Xiao |first1=Guang-Yao |last2=Liu |first2=Yu-Juan |display-authors=etal |date=May 2023 |title=The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements |journal=Research in Astronomy and Astrophysics |volume=23 |issue=5 |pages=055022 |doi=10.1088/1674-4527/accb7e |arxiv=2303.12409 |bibcode=2023RAA....23e5022X}}
}}
{{Sky|13|29|21.1137|-|35|34|15.589|108}}
{{Stars of Centaurus}}
{{DEFAULTSORT:HD 117207}}
Category:G-type main-sequence stars