HD 207832#Planetary system

{{Starbox begin

|name=HD 207832

}}

{{Starbox observe

| epoch = J2000

| constell = Piscis Austrinus

| ra = {{RA|21|52|36.2810}}

| dec = {{DEC|-26|01|35.6133}}

| appmag_v = 8.79

}}

{{Starbox character

| type = main-sequence star

| class = G5V{{citation|arxiv=1809.01228|year=2018|title=Radial velocities from the N2K Project: 6 new cold gas giant planets orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810|doi=10.3847/1538-3881/aae1f5|last1=Ment|first1=Kristo|last2=Fischer|first2=Debra A.|last3=Bakos|first3=Gaspar|last4=Howard|first4=Andrew W.|last5=Isaacson|first5=Howard|journal=The Astronomical Journal|volume=156|issue=5|page=213|bibcode=2018AJ....156..213M|s2cid=119243619 |doi-access=free }}

}}

{{Starbox astrometry

| radial_v = -16.481{{±|0.185}}{{cite Gaia EDR3|6812056381881853056}}

| prop_mo_ra = 129.310

| prop_mo_dec = -143.132

| parallax = 16.8897

| p_error = 0.0151

| parallax_footnote =

}}

{{Starbox detail

| source =

| mass = 1.08{{±|0.01}}

| radius = 0.97{{±|0.02}}

| temperature = 5764{{±|15}}

| luminosity = 0.78{{±|0.09}}

| gravity = 4.61{{±|0.04}}

| metal_fe = 0.17{{±|0.01}}

| rotation = 17.8 d

| rotational_velocity =

| age_gyr = 0.74{{±|0.62}}

}}

{{Starbox catalog

| names = {{odlist|CD=-26 15858|2MASS = J21523626-2601352|TYC=6589-761-1|HIP=107985|GSC=06956-00378}}{{cite simbad|title=HD 207832|accessdate=2021-01-20}}

}}

{{Starbox reference

| Simbad = HD+207832

}}

HD 207832 is a G-type main-sequence star. Its surface temperature is 5764{{±|15}} K. HD 207832 is slightly enriched compared to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.17{{±|0.01}} and is much younger at an age of 0.74{{±|0.62}} billion years. Kinematically, it belongs to the thin disk of the Milky Way.{{citation|arxiv=1712.01035|year=2018|title=Chemical fingerprints of hot Jupiter planet formation|doi=10.1051/0004-6361/201732001|last1=Maldonado|first1=J.|last2=Villaver|first2=E.|last3=Eiroa|first3=C.|journal=Astronomy & Astrophysics|volume=612|pages=A93|bibcode=2018A&A...612A..93M|s2cid=119458710}}

A multiplicity study in 2014 detected a candidate comoving stellar companion - a red dwarf star or brown dwarf with a spectral class M6.5, at a very wide projected separation of 38.57′ (2.0 light years){{citation|arxiv=1408.1208|year=2014|title=Binary frequency of planet-host stars at wide separations. A new brown dwarf companion to a planet-host star|doi=10.1051/0004-6361/201424210|last1=Lodieu|first1=N.|last2=Perez-Garrido|first2=A.|last3=Bejar|first3=V. J. S.|last4=Gauza|first4=B.|last5=Ruiz|first5=M. T.|last6=Rebolo|first6=R.|last7=Pinfield|first7=D. J.|last8=Martin|first8=E. L.|journal=Astronomy & Astrophysics|volume=A120|page=569|bibcode=2014A&A...569A.120L|s2cid=118516214}}

Planetary system

In 2012, two planets, named HD 207832 b and HD 207832 c, were discovered by the radial velocity method on wide, eccentric orbits. The planetary system would remain stable even if the planetary orbits are coplanar.{{citation|arxiv=1706.00084|year=2017|title=Moderately eccentric warm Jupiters from secular interactions with exterior companions|doi=10.1093/mnras/stx2250|last1=Anderson|first1=Kassandra R.|last2=Lai|first2=Dong|journal=Monthly Notices of the Royal Astronomical Society|volume=472|issue=3|pages=3692–3705|doi-access=free |bibcode=2017MNRAS.472.3692A|s2cid=119260335}}

Although discovery of the inner planet was confirmed in 2018, the discovery of both planets was suspected to be a false positive in 2020, as newer radial velocity data do not support the existence of the planets.{{citation|arxiv=2004.13734|year=2020|title=Astrophysical Insights into Radial Velocity Jitter from an Analysis of 600 Planet-search Stars|doi=10.3847/1538-3881/ab855a|last1=Luhn|first1=Jacob K.|last2=Wright|first2=Jason T.|last3=Howard|first3=Andrew W.|last4=Isaacson|first4=Howard|journal=The Astronomical Journal|volume=159|issue=5|page=235|bibcode=2020AJ....159..235L|s2cid=216642215 |doi-access=free }}

{{OrbitboxPlanet begin

| name = HD 207832

| table_ref ={{citation|arxiv=1207.2806|year=2012|title=The Lick-Carnegie Survey: A New Two-Planet System Around the Star HD 207832|doi=10.1088/0004-637X/756/1/91|last1=Haghighipour|first1=Nader|last2=Butler|first2=R. Paul|last3=Rivera|first3=Eugenio J.|last4=Henry|first4=Gregory W.|last5=Vogt|first5=Steven S.|journal=The Astrophysical Journal|volume=756|issue=1|page=91|bibcode=2012ApJ...756...91H|s2cid=1137984}}

}}

{{OrbitboxPlanet hypothetical

| exoplanet = b

| mass = ≥ 0.56{{±|0.091}}

| radius =

| semimajor = 0.586{{±|0.032}}

| period = 160.07{{±|0.23}}

| eccentricity = 0.197{{±|0.053}}

| inclination =

}}

{{OrbitboxPlanet hypothetical

| exoplanet = c