| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Hydra |
| Right ascension | 08h 42m 25.12195s [1] |
| Declination | +04° 34′ 41.1457″ [1] |
| Apparent magnitude (V) | +7.614 [2] |
| Characteristics | |
| Spectral type | G0V |
| U−B color index | ? |
| B−V color index | 0.581 [2] |
| V−R color index | 0.4 |
| R−I color index | 0.2 |
| Variable type | “None” |
| Astrometry | |
| Radial velocity (Rv) | 3.90±0.13 [1] km/s |
| Proper motion (μ) |
RA: 24.666±0.025
mas/
yr
[1] Dec.: −200.238±0.019 mas/ yr [1] |
| Parallax (π) | 17.4242 ± 0.0247 mas [1] |
| Distance | 187.2 ± 0.3
ly (57.39 ± 0.08 pc) |
| Absolute magnitude (MV) | +3.57 ± 0.15 |
| Details | |
| Mass | 1.24 [2] M☉ |
| Radius | 1.64 ± 0.19 [2] R☉ |
| Luminosity (bolometric) | 3.037 ± 0.485 [2] L☉ |
| Surface gravity (log g) | 4.4 ± 0.15 [2] cgs |
| Temperature | 5960 ± 100 [2] K |
| Metallicity [Fe/H] | +0.13 [2] dex |
| Rotational velocity (v sin i) | 4.3 [2] km/s |
| Age | 3.7 ± 0.4 [2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 74156 is a yellow dwarf star ( spectral type G0V) in the constellation of Hydra, 187 light years from the Solar System. [1] It is known to be orbited by two giant planets.
This star is 24% more massive and 64% larger than the Sun. The total luminosity is 2.96 times that of the Sun and its temperature 5960 K. [2] The age of the star is estimated at 3.7 billion years, [2] with metallicity 1.35 times that of the Sun based on its abundance of iron.
In April 2001, two giant planets were announced orbiting the star. [3] [4] The first planet HD 74156 b orbits the star at a distance closer than Mercury is to the Sun, in an extremely eccentric orbit. The second planet HD 74156 c is a long-period, massive planet (at least 8 times the mass of Jupiter), which orbits the star in an elliptical orbit with a semimajor axis of 3.90 astronomical units. [2] In 2022, the inclination and true mass of HD 74156 c were measured via astrometry. [5]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.778±0.020 MJ | 0.2916±0.0033 | 51.6385±0.0015 | 0.6380±0.0061 | — | — |
| c | 8.665+1.385 −0.470 MJ |
3.678+0.145 −0.159 |
2448.5±4.2 | 0.377±0.006 | 120.162+7.601 −66.225 ° |
— |
Given the two-planet configuration of the system under the assumption that the orbits are coplanar and have masses equal to their minimum masses, an additional Saturn-mass planet would be stable in a region between 0.9 and 1.4 AU between the orbits of the two known planets. [7] Under the "packed planetary systems" hypothesis, which predicts that planetary systems form in such a way that the system could not support additional planets between the orbits of the existing ones, the gap would be expected to host a planet.
In September 2007, a third planet with a mass at least 0.396 Jupiter masses was announced to be orbiting between planets b and c with an eccentric orbit. [8] The planet, orbiting in a region of the planetary system previously known to be stable for additional planets, was seen as a confirmation of the "packed planetary systems" hypothesis. [9] However, Roman V. Baluev has cast doubt on this discovery, suggesting that the observed variations may be due to annual errors in the data. [10] A subsequent search using the Hobby-Eberly Telescope also failed to confirm the planet, [11] and further data obtained using HIRES instrument strongly contradicts its existence. [2]
- ^ a b c d e f 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.
- ^ a b c d e f g h i j k l m n Meschiari, Stefano; et al. (2011). "The Lick-Carnegie Survey: Four New Exoplanet Candidates". The Astrophysical Journal. 727 (2). 117. arXiv: 1011.4068. Bibcode: 2011ApJ...727..117M. doi: 10.1088/0004-637X/727/2/117. S2CID 59065004.
- ^ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 27, 2012.
- ^ Naef, Dominique; Mayor, Michel; Beuzit, Jean-Luc; Perrier, Christian; Queloz, Didier; Sivan, Jean-Pierre; Udry, Stéphane (2004). "The ELODIE survey for northern extra-solar planets. III. Three planetary candidates detected with ELODIE" (PDF). Astronomy and Astrophysics. 414 (1): 351–359. arXiv: astro-ph/0310261. Bibcode: 2004A&A...414..351N. doi: 10.1051/0004-6361:20034091. S2CID 16603563.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv: 2208.12720. Bibcode: 2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57. S2CID 251864022.
- ^ Feng, Y. Katherina; et al. (2015). "The California Planet Survey IV: A Planet Orbiting the Giant Star HD 145934 and Updates to Seven Systems with Long-period Planets". The Astrophysical Journal. 800 (1). 22. arXiv: 1501.00633. Bibcode: 2015ApJ...800...22F. doi: 10.1088/0004-637X/800/1/22. S2CID 56390823.
- ^ Sean N. Raymond; Rory Barnes (2005). "Predicting Planets in Known Extrasolar Planetary Systems. II. Testing for Saturn Mass Planets". The Astrophysical Journal. 619 (1): 549–557. arXiv: astro-ph/0404211. Bibcode: 2005ApJ...619..549R. doi: 10.1086/426311. S2CID 13015545.
- ^ Jacob L. Bean; et al. (2008). "Detection of a Third Planet in the HD 74156 System Using the Hobby-Eberly Telescope". The Astrophysical Journal. 672 (2): 1202–1208. arXiv: 0709.1656. Bibcode: 2008ApJ...672.1202B. doi: 10.1086/523701. hdl: 2152/35107. S2CID 15507937.
- ^ Barnes, Rory; et al. (2008). "The Successful Prediction of the Extrasolar Planet HD 74156 d". The Astrophysical Journal Letters. 680 (1): L57–L60. arXiv: 0804.4496. Bibcode: 2008ApJ...680L..57B. doi: 10.1086/589712. S2CID 14070540.
- ^ Baluev, Roman V. (2008). "Accounting for velocity jitters in planet search surveys". Monthly Notices of the Royal Astronomical Society. 393 (3): 969–978. arXiv: 0712.3862. Bibcode: 2009MNRAS.393..969B. doi: 10.1111/j.1365-2966.2008.14217.x. S2CID 15170720.
- ^ Wittenmyer, Robert A.; Endl, Michael; Cochran, William D.; Levison, Harold F.; Henry, Gregory W. (2009). "A Search for Multi-Planet Systems Using the Hobby-Eberly Telescope". The Astrophysical Journal Supplement. 182 (1): 97–119. arXiv: 0903.0652. Bibcode: 2009ApJS..182...97W. doi: 10.1088/0067-0049/182/1/97. S2CID 7422668.
- "Notes for star HD 74156". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007.
- Extrasolar Planet Interactions Archived 2016-05-05 at the Wayback Machine by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Hydra |
| Right ascension | 08h 42m 25.12195s [1] |
| Declination | +04° 34′ 41.1457″ [1] |
| Apparent magnitude (V) | +7.614 [2] |
| Characteristics | |
| Spectral type | G0V |
| U−B color index | ? |
| B−V color index | 0.581 [2] |
| V−R color index | 0.4 |
| R−I color index | 0.2 |
| Variable type | “None” |
| Astrometry | |
| Radial velocity (Rv) | 3.90±0.13 [1] km/s |
| Proper motion (μ) |
RA: 24.666±0.025
mas/
yr
[1] Dec.: −200.238±0.019 mas/ yr [1] |
| Parallax (π) | 17.4242 ± 0.0247 mas [1] |
| Distance | 187.2 ± 0.3
ly (57.39 ± 0.08 pc) |
| Absolute magnitude (MV) | +3.57 ± 0.15 |
| Details | |
| Mass | 1.24 [2] M☉ |
| Radius | 1.64 ± 0.19 [2] R☉ |
| Luminosity (bolometric) | 3.037 ± 0.485 [2] L☉ |
| Surface gravity (log g) | 4.4 ± 0.15 [2] cgs |
| Temperature | 5960 ± 100 [2] K |
| Metallicity [Fe/H] | +0.13 [2] dex |
| Rotational velocity (v sin i) | 4.3 [2] km/s |
| Age | 3.7 ± 0.4 [2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 74156 is a yellow dwarf star ( spectral type G0V) in the constellation of Hydra, 187 light years from the Solar System. [1] It is known to be orbited by two giant planets.
This star is 24% more massive and 64% larger than the Sun. The total luminosity is 2.96 times that of the Sun and its temperature 5960 K. [2] The age of the star is estimated at 3.7 billion years, [2] with metallicity 1.35 times that of the Sun based on its abundance of iron.
In April 2001, two giant planets were announced orbiting the star. [3] [4] The first planet HD 74156 b orbits the star at a distance closer than Mercury is to the Sun, in an extremely eccentric orbit. The second planet HD 74156 c is a long-period, massive planet (at least 8 times the mass of Jupiter), which orbits the star in an elliptical orbit with a semimajor axis of 3.90 astronomical units. [2] In 2022, the inclination and true mass of HD 74156 c were measured via astrometry. [5]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.778±0.020 MJ | 0.2916±0.0033 | 51.6385±0.0015 | 0.6380±0.0061 | — | — |
| c | 8.665+1.385 −0.470 MJ |
3.678+0.145 −0.159 |
2448.5±4.2 | 0.377±0.006 | 120.162+7.601 −66.225 ° |
— |
Given the two-planet configuration of the system under the assumption that the orbits are coplanar and have masses equal to their minimum masses, an additional Saturn-mass planet would be stable in a region between 0.9 and 1.4 AU between the orbits of the two known planets. [7] Under the "packed planetary systems" hypothesis, which predicts that planetary systems form in such a way that the system could not support additional planets between the orbits of the existing ones, the gap would be expected to host a planet.
In September 2007, a third planet with a mass at least 0.396 Jupiter masses was announced to be orbiting between planets b and c with an eccentric orbit. [8] The planet, orbiting in a region of the planetary system previously known to be stable for additional planets, was seen as a confirmation of the "packed planetary systems" hypothesis. [9] However, Roman V. Baluev has cast doubt on this discovery, suggesting that the observed variations may be due to annual errors in the data. [10] A subsequent search using the Hobby-Eberly Telescope also failed to confirm the planet, [11] and further data obtained using HIRES instrument strongly contradicts its existence. [2]
- ^ a b c d e f 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.
- ^ a b c d e f g h i j k l m n Meschiari, Stefano; et al. (2011). "The Lick-Carnegie Survey: Four New Exoplanet Candidates". The Astrophysical Journal. 727 (2). 117. arXiv: 1011.4068. Bibcode: 2011ApJ...727..117M. doi: 10.1088/0004-637X/727/2/117. S2CID 59065004.
- ^ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 27, 2012.
- ^ Naef, Dominique; Mayor, Michel; Beuzit, Jean-Luc; Perrier, Christian; Queloz, Didier; Sivan, Jean-Pierre; Udry, Stéphane (2004). "The ELODIE survey for northern extra-solar planets. III. Three planetary candidates detected with ELODIE" (PDF). Astronomy and Astrophysics. 414 (1): 351–359. arXiv: astro-ph/0310261. Bibcode: 2004A&A...414..351N. doi: 10.1051/0004-6361:20034091. S2CID 16603563.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv: 2208.12720. Bibcode: 2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57. S2CID 251864022.
- ^ Feng, Y. Katherina; et al. (2015). "The California Planet Survey IV: A Planet Orbiting the Giant Star HD 145934 and Updates to Seven Systems with Long-period Planets". The Astrophysical Journal. 800 (1). 22. arXiv: 1501.00633. Bibcode: 2015ApJ...800...22F. doi: 10.1088/0004-637X/800/1/22. S2CID 56390823.
- ^ Sean N. Raymond; Rory Barnes (2005). "Predicting Planets in Known Extrasolar Planetary Systems. II. Testing for Saturn Mass Planets". The Astrophysical Journal. 619 (1): 549–557. arXiv: astro-ph/0404211. Bibcode: 2005ApJ...619..549R. doi: 10.1086/426311. S2CID 13015545.
- ^ Jacob L. Bean; et al. (2008). "Detection of a Third Planet in the HD 74156 System Using the Hobby-Eberly Telescope". The Astrophysical Journal. 672 (2): 1202–1208. arXiv: 0709.1656. Bibcode: 2008ApJ...672.1202B. doi: 10.1086/523701. hdl: 2152/35107. S2CID 15507937.
- ^ Barnes, Rory; et al. (2008). "The Successful Prediction of the Extrasolar Planet HD 74156 d". The Astrophysical Journal Letters. 680 (1): L57–L60. arXiv: 0804.4496. Bibcode: 2008ApJ...680L..57B. doi: 10.1086/589712. S2CID 14070540.
- ^ Baluev, Roman V. (2008). "Accounting for velocity jitters in planet search surveys". Monthly Notices of the Royal Astronomical Society. 393 (3): 969–978. arXiv: 0712.3862. Bibcode: 2009MNRAS.393..969B. doi: 10.1111/j.1365-2966.2008.14217.x. S2CID 15170720.
- ^ Wittenmyer, Robert A.; Endl, Michael; Cochran, William D.; Levison, Harold F.; Henry, Gregory W. (2009). "A Search for Multi-Planet Systems Using the Hobby-Eberly Telescope". The Astrophysical Journal Supplement. 182 (1): 97–119. arXiv: 0903.0652. Bibcode: 2009ApJS..182...97W. doi: 10.1088/0067-0049/182/1/97. S2CID 7422668.
- "Notes for star HD 74156". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007.
- Extrasolar Planet Interactions Archived 2016-05-05 at the Wayback Machine by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona