| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 12m 31.47875s [1] |
| Declination | +51° 46′ 43.5637″ [1] |
| Apparent magnitude (V) | 11.83 |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | G |
| Astrometry | |
| Radial velocity (Rv) | −21.91±0.69 [1] km/s |
| Proper motion (μ) |
RA: -9.972
mas/
yr
[1] Dec.: 1.790 mas/ yr [1] |
| Parallax (π) | 3.1358 ± 0.0201 mas [1] |
| Distance | 1,040 ± 7
ly (319 ± 2 pc) |
| Orbit [2] | |
| Primary | HAT-P-29 |
| Companion | HAT-P-29 B |
| Semi-major axis (a) | 3.290±0.002" (1041 AU) |
| Details [3] | |
| Mass | 1.198+0.065 −0.063 M☉ |
| Radius | 1.229+0.080 −0.073 R☉ |
| Luminosity | 1.89+0.3 −0.25 L☉ |
| Surface gravity (log g) | 4.337+0.045 −0.045 cgs |
| Temperature | 6112±88 K |
| Metallicity [Fe/H] | 0.128+0.079 −0.080 dex |
| Age | 2.2±1.0 [4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HAT-P-29, also known as Muspelheim since 2019 (as part of the IAU's NameExoWorlds project), [6] is a star about 1,040 light-years (320 parsecs) away. It is a G-type main-sequence star. The star's age of 2.2±1.0 billion years is less than half that of the Sun. [4] HAT-P-29 is slightly enriched in heavy elements, having 35% more iron than the Sun.
A very faint 19th-magnitude stellar companion was detected in 2016 at a projected separation of 3.290±0.002″, [2] but Gaia DR2 astrometry suggests that this is an unrelated background object. [7]
Planetary system
In 2011 a transiting hot Jupiter planet, HAT-P-29b, was detected on a mildly eccentric orbit. [4] The planet was named " Surt" by Denmark in 2019. [8] The planetary orbit is likely aligned with the equatorial plane of the star, with a misalignment equal to 26±16 degrees. [9]
In 2018, a transit-timing variation survey indicated additional planets with masses exceeding approximately half of Earth are absent in the system. [3]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Surt) | 0.767+0.046 −0.045 MJ |
0.0665±0.0012 | 5.723376±0.000021 | 0.073+0.029 −0.028 |
88.06+0.78 −0.59 ° |
1.055+0.079 −0.072 RJ |
References
- ^ 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.
- ^ a b Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Bryan, Marta; Crepp, Justin R.; Batygin, Konstantin; Crossfield, Ian; Hansen, Brad; Howard, Andrew W.; Johnson, John A.; Mawet, Dimitri; Morton, Timothy D.; Muirhead, Philip S.; Wang, Ji (2016), "FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION", The Astrophysical Journal, 827 (1): 8, arXiv: 1606.07102, Bibcode: 2016ApJ...827....8N, doi: 10.3847/0004-637X/827/1/8, S2CID 41083068
- ^ a b c Wang, Songhu; Wang, Xian-Yu; Wang, Yong-Hao; Liu, Hui-Gen; Hinse, Tobias C.; Eastman, Jason; Bayliss, Daniel; Hori, Yasunori; Hu, Shao-Ming; Li, Kai; Liu, Jinzhong; Narita, Norio; Peng, Xiyan; Wittenmyer, R. A.; Wu, Zhen-Yu; Zhang, Hui; Zhang, Xiaojia; Zhao, Haibin; Zhou, Ji-Lin; Zhou, George; Zhou, Xu; Laughlin, Gregory (2018), "Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b", The Astronomical Journal, 156 (4): 181, arXiv: 1807.10107, Bibcode: 2018AJ....156..181W, doi: 10.3847/1538-3881/aadcfc, S2CID 119415237
- ^ a b c Buchhave, L. A.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Latham, D. W.; Andersen, J.; Kovács, G.; Noyes, R. W.; Shporer, A.; Esquerdo, G. A.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Béky, B.; Sasselov, D. D.; Fűrész, G.; Quinn, S. N.; Stefanik, R. P.; Szklenár, T.; Berlind, P.; Calkins, M. L.; Lázár, J.; Papp, I.; Sári, P. (2011), "HAT-P-28b AND HAT-P-29b: TWO SUB-JUPITER MASS TRANSITING PLANETS", The Astrophysical Journal, 733 (2): 116, arXiv: 1103.1813, Bibcode: 2011ApJ...733..116B, doi: 10.1088/0004-637X/733/2/116, S2CID 119293967
- ^ "HAT-P-29". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ IAU100 NameExoWorlds APPROVED NAMES
- ^ Mugrauer, M.; et al. (2019). "Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release". Monthly Notices of the Royal Astronomical Society. 490 (4): 5088. Bibcode: 2019MNRAS.490.5088M. doi: 10.1093/mnras/stz2673.
- ^ Denmark names new planet after Norse fire giant Surt
- ^ Mancini, L.; et al. (2022), "The GAPS Programme at TNG", Astronomy & Astrophysics, 664: A162, arXiv: 2205.10549, doi: 10.1051/0004-6361/202243742, S2CID 248986121
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 | This extrasolar-planet-related article is a stub. You can help Wikipedia by expanding it. |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 12m 31.47875s [1] |
| Declination | +51° 46′ 43.5637″ [1] |
| Apparent magnitude (V) | 11.83 |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | G |
| Astrometry | |
| Radial velocity (Rv) | −21.91±0.69 [1] km/s |
| Proper motion (μ) |
RA: -9.972
mas/
yr
[1] Dec.: 1.790 mas/ yr [1] |
| Parallax (π) | 3.1358 ± 0.0201 mas [1] |
| Distance | 1,040 ± 7
ly (319 ± 2 pc) |
| Orbit [2] | |
| Primary | HAT-P-29 |
| Companion | HAT-P-29 B |
| Semi-major axis (a) | 3.290±0.002" (1041 AU) |
| Details [3] | |
| Mass | 1.198+0.065 −0.063 M☉ |
| Radius | 1.229+0.080 −0.073 R☉ |
| Luminosity | 1.89+0.3 −0.25 L☉ |
| Surface gravity (log g) | 4.337+0.045 −0.045 cgs |
| Temperature | 6112±88 K |
| Metallicity [Fe/H] | 0.128+0.079 −0.080 dex |
| Age | 2.2±1.0 [4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HAT-P-29, also known as Muspelheim since 2019 (as part of the IAU's NameExoWorlds project), [6] is a star about 1,040 light-years (320 parsecs) away. It is a G-type main-sequence star. The star's age of 2.2±1.0 billion years is less than half that of the Sun. [4] HAT-P-29 is slightly enriched in heavy elements, having 35% more iron than the Sun.
A very faint 19th-magnitude stellar companion was detected in 2016 at a projected separation of 3.290±0.002″, [2] but Gaia DR2 astrometry suggests that this is an unrelated background object. [7]
Planetary system
In 2011 a transiting hot Jupiter planet, HAT-P-29b, was detected on a mildly eccentric orbit. [4] The planet was named " Surt" by Denmark in 2019. [8] The planetary orbit is likely aligned with the equatorial plane of the star, with a misalignment equal to 26±16 degrees. [9]
In 2018, a transit-timing variation survey indicated additional planets with masses exceeding approximately half of Earth are absent in the system. [3]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Surt) | 0.767+0.046 −0.045 MJ |
0.0665±0.0012 | 5.723376±0.000021 | 0.073+0.029 −0.028 |
88.06+0.78 −0.59 ° |
1.055+0.079 −0.072 RJ |
References
- ^ 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.
- ^ a b Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Bryan, Marta; Crepp, Justin R.; Batygin, Konstantin; Crossfield, Ian; Hansen, Brad; Howard, Andrew W.; Johnson, John A.; Mawet, Dimitri; Morton, Timothy D.; Muirhead, Philip S.; Wang, Ji (2016), "FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION", The Astrophysical Journal, 827 (1): 8, arXiv: 1606.07102, Bibcode: 2016ApJ...827....8N, doi: 10.3847/0004-637X/827/1/8, S2CID 41083068
- ^ a b c Wang, Songhu; Wang, Xian-Yu; Wang, Yong-Hao; Liu, Hui-Gen; Hinse, Tobias C.; Eastman, Jason; Bayliss, Daniel; Hori, Yasunori; Hu, Shao-Ming; Li, Kai; Liu, Jinzhong; Narita, Norio; Peng, Xiyan; Wittenmyer, R. A.; Wu, Zhen-Yu; Zhang, Hui; Zhang, Xiaojia; Zhao, Haibin; Zhou, Ji-Lin; Zhou, George; Zhou, Xu; Laughlin, Gregory (2018), "Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b", The Astronomical Journal, 156 (4): 181, arXiv: 1807.10107, Bibcode: 2018AJ....156..181W, doi: 10.3847/1538-3881/aadcfc, S2CID 119415237
- ^ a b c Buchhave, L. A.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Latham, D. W.; Andersen, J.; Kovács, G.; Noyes, R. W.; Shporer, A.; Esquerdo, G. A.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Béky, B.; Sasselov, D. D.; Fűrész, G.; Quinn, S. N.; Stefanik, R. P.; Szklenár, T.; Berlind, P.; Calkins, M. L.; Lázár, J.; Papp, I.; Sári, P. (2011), "HAT-P-28b AND HAT-P-29b: TWO SUB-JUPITER MASS TRANSITING PLANETS", The Astrophysical Journal, 733 (2): 116, arXiv: 1103.1813, Bibcode: 2011ApJ...733..116B, doi: 10.1088/0004-637X/733/2/116, S2CID 119293967
- ^ "HAT-P-29". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ IAU100 NameExoWorlds APPROVED NAMES
- ^ Mugrauer, M.; et al. (2019). "Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release". Monthly Notices of the Royal Astronomical Society. 490 (4): 5088. Bibcode: 2019MNRAS.490.5088M. doi: 10.1093/mnras/stz2673.
- ^ Denmark names new planet after Norse fire giant Surt
- ^ Mancini, L.; et al. (2022), "The GAPS Programme at TNG", Astronomy & Astrophysics, 664: A162, arXiv: 2205.10549, doi: 10.1051/0004-6361/202243742, S2CID 248986121
| Stars |
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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
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|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||
|
| This main-sequence-star-related article is a stub. You can help Wikipedia by expanding it. |
|
| This extrasolar-planet-related article is a stub. You can help Wikipedia by expanding it. |