| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Piscis Austrinus |
| Right ascension | 21h 52m 36.2810s [1] |
| Declination | −26° 01′ 35.6133″ [1] |
| Apparent magnitude (V) | 8.79 |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | G5V [2] |
| Astrometry | |
| Radial velocity (Rv) | -16.481±0.185 [3] km/s |
| Proper motion (μ) |
RA: 129.310
[3]
mas/
yr Dec.: -143.132 [3] mas/ yr |
| Parallax (π) | 16.8897 ± 0.0151 mas [3] |
| Distance | 193.1 ± 0.2
ly (59.21 ± 0.05 pc) |
| Details [4] | |
| Mass | 1.08±0.01 M☉ |
| Radius | 0.97±0.02 R☉ |
| Luminosity | 0.78±0.09 [2] L☉ |
| Surface gravity (log g) | 4.61±0.04 cgs |
| Temperature | 5764±15 K |
| Metallicity [Fe/H] | 0.17±0.01 dex |
| Rotation | 17.8 d [5] |
| Age | 0.74±0.62 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 207832 is a G-type main-sequence star. Its surface temperature is 5764±15 K. [4] 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. [4]
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) [6]
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. [5] The planetary system would remain stable even if the planetary orbits are coplanar. [7]
Although discovery of the inner planet was confirmed [2] 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. [8]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥ 0.56±0.091 MJ | 0.586±0.032 | 160.07±0.23 | 0.197±0.053 | — | — |
| c (unconfirmed) | ≥0.73+0.18 −0.05 M🜨 |
2.112+0.087 −0.045 |
1155.7+71.9 −37.0 |
0.27+0.22 −0.10 |
— | — |
References
- ^ a b c "HD 207832". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-20.
- ^ a b c d Ment, Kristo; Fischer, Debra A.; Bakos, Gaspar; Howard, Andrew W.; Isaacson, Howard (2018), "Radial velocities from the N2K Project: 6 new cold gas giant planets orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810", The Astronomical Journal, 156 (5): 213, arXiv: 1809.01228, Bibcode: 2018AJ....156..213M, doi: 10.3847/1538-3881/aae1f5, S2CID 119243619
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Maldonado, J.; Villaver, E.; Eiroa, C. (2018), "Chemical fingerprints of hot Jupiter planet formation", Astronomy & Astrophysics, 612: A93, arXiv: 1712.01035, Bibcode: 2018A&A...612A..93M, doi: 10.1051/0004-6361/201732001, S2CID 119458710
- ^ a b c Haghighipour, Nader; Butler, R. Paul; Rivera, Eugenio J.; Henry, Gregory W.; Vogt, Steven S. (2012), "The Lick-Carnegie Survey: A New Two-Planet System Around the Star HD 207832", The Astrophysical Journal, 756 (1): 91, arXiv: 1207.2806, Bibcode: 2012ApJ...756...91H, doi: 10.1088/0004-637X/756/1/91, S2CID 1137984
- ^ Lodieu, N.; Perez-Garrido, A.; Bejar, V. J. S.; Gauza, B.; Ruiz, M. T.; Rebolo, R.; Pinfield, D. J.; Martin, E. L. (2014), "Binary frequency of planet-host stars at wide separations. A new brown dwarf companion to a planet-host star", Astronomy & Astrophysics, A120: 569, arXiv: 1408.1208, Bibcode: 2014A&A...569A.120L, doi: 10.1051/0004-6361/201424210, S2CID 118516214
- ^ Anderson, Kassandra R.; Lai, Dong (2017), "Moderately eccentric warm Jupiters from secular interactions with exterior companions", Monthly Notices of the Royal Astronomical Society, 472 (3): 3692–3705, arXiv: 1706.00084, Bibcode: 2017MNRAS.472.3692A, doi: 10.1093/mnras/stx2250, S2CID 119260335
- ^ Luhn, Jacob K.; Wright, Jason T.; Howard, Andrew W.; Isaacson, Howard (2020), "Astrophysical Insights into Radial Velocity Jitter from an Analysis of 600 Planet-search Stars", The Astronomical Journal, 159 (5): 235, arXiv: 2004.13734, Bibcode: 2020AJ....159..235L, doi: 10.3847/1538-3881/ab855a, S2CID 216642215
| Stars |
| ||||||||
|---|---|---|---|---|---|---|---|---|---|
| |||||||||
| Galaxies |
| ||||||||
| |||||||||
| |||||||||
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Piscis Austrinus |
| Right ascension | 21h 52m 36.2810s [1] |
| Declination | −26° 01′ 35.6133″ [1] |
| Apparent magnitude (V) | 8.79 |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | G5V [2] |
| Astrometry | |
| Radial velocity (Rv) | -16.481±0.185 [3] km/s |
| Proper motion (μ) |
RA: 129.310
[3]
mas/
yr Dec.: -143.132 [3] mas/ yr |
| Parallax (π) | 16.8897 ± 0.0151 mas [3] |
| Distance | 193.1 ± 0.2
ly (59.21 ± 0.05 pc) |
| Details [4] | |
| Mass | 1.08±0.01 M☉ |
| Radius | 0.97±0.02 R☉ |
| Luminosity | 0.78±0.09 [2] L☉ |
| Surface gravity (log g) | 4.61±0.04 cgs |
| Temperature | 5764±15 K |
| Metallicity [Fe/H] | 0.17±0.01 dex |
| Rotation | 17.8 d [5] |
| Age | 0.74±0.62 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 207832 is a G-type main-sequence star. Its surface temperature is 5764±15 K. [4] 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. [4]
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) [6]
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. [5] The planetary system would remain stable even if the planetary orbits are coplanar. [7]
Although discovery of the inner planet was confirmed [2] 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. [8]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥ 0.56±0.091 MJ | 0.586±0.032 | 160.07±0.23 | 0.197±0.053 | — | — |
| c (unconfirmed) | ≥0.73+0.18 −0.05 M🜨 |
2.112+0.087 −0.045 |
1155.7+71.9 −37.0 |
0.27+0.22 −0.10 |
— | — |
References
- ^ a b c "HD 207832". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-20.
- ^ a b c d Ment, Kristo; Fischer, Debra A.; Bakos, Gaspar; Howard, Andrew W.; Isaacson, Howard (2018), "Radial velocities from the N2K Project: 6 new cold gas giant planets orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810", The Astronomical Journal, 156 (5): 213, arXiv: 1809.01228, Bibcode: 2018AJ....156..213M, doi: 10.3847/1538-3881/aae1f5, S2CID 119243619
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv: 2012.01533. Bibcode: 2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Maldonado, J.; Villaver, E.; Eiroa, C. (2018), "Chemical fingerprints of hot Jupiter planet formation", Astronomy & Astrophysics, 612: A93, arXiv: 1712.01035, Bibcode: 2018A&A...612A..93M, doi: 10.1051/0004-6361/201732001, S2CID 119458710
- ^ a b c Haghighipour, Nader; Butler, R. Paul; Rivera, Eugenio J.; Henry, Gregory W.; Vogt, Steven S. (2012), "The Lick-Carnegie Survey: A New Two-Planet System Around the Star HD 207832", The Astrophysical Journal, 756 (1): 91, arXiv: 1207.2806, Bibcode: 2012ApJ...756...91H, doi: 10.1088/0004-637X/756/1/91, S2CID 1137984
- ^ Lodieu, N.; Perez-Garrido, A.; Bejar, V. J. S.; Gauza, B.; Ruiz, M. T.; Rebolo, R.; Pinfield, D. J.; Martin, E. L. (2014), "Binary frequency of planet-host stars at wide separations. A new brown dwarf companion to a planet-host star", Astronomy & Astrophysics, A120: 569, arXiv: 1408.1208, Bibcode: 2014A&A...569A.120L, doi: 10.1051/0004-6361/201424210, S2CID 118516214
- ^ Anderson, Kassandra R.; Lai, Dong (2017), "Moderately eccentric warm Jupiters from secular interactions with exterior companions", Monthly Notices of the Royal Astronomical Society, 472 (3): 3692–3705, arXiv: 1706.00084, Bibcode: 2017MNRAS.472.3692A, doi: 10.1093/mnras/stx2250, S2CID 119260335
- ^ Luhn, Jacob K.; Wright, Jason T.; Howard, Andrew W.; Isaacson, Howard (2020), "Astrophysical Insights into Radial Velocity Jitter from an Analysis of 600 Planet-search Stars", The Astronomical Journal, 159 (5): 235, arXiv: 2004.13734, Bibcode: 2020AJ....159..235L, doi: 10.3847/1538-3881/ab855a, S2CID 216642215
| Stars |
| ||||||||
|---|---|---|---|---|---|---|---|---|---|
| |||||||||
| Galaxies |
| ||||||||
| |||||||||
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