HD 113337 B
HD 113337 (LDS 2662 A) is the primary component of binary star system LDS 2662, about 118 light-years away from Earth. The primary main-sequence star belongs to the spectral class of F6. The star system is extremely young, and it is slightly enriched in heavy elements, with an abundance of such elements at about 115% that of the Sun.
The primary star is surrounded by a debris disk discovered by the Herschel Space Observatory, and the plane of the disk is likely misaligned with the planetary orbits by 17–32°. The effective temperature of this disk is 55 K.
The possibility of other stellar companions near the primary star was ruled out in 2016, for projected separations above 5″ (181 AU).
The existence of a secondary companion (called LDS 2662 B, or LSPM J1301+6337) was discovered in 2001 and confirmed to be bound to the primary in 2007. Initially believed to be a single red dwarf star, in 2012 the companion was discovered to actually be a pair of nearly identical red dwarfs, of spectral class M3.5, orbiting each other at a distance of 7.2±2.6 AU, with a period of 39 years.
Planetary system
In 2013, one superjovian planet, HD 113337 b, was discovered, via the radial velocity method, on an eccentric orbit around HD 113337. Another giant planet or brown dwarf candidate, HD 113337 c, has been suspected since 2018, with the evidence for its existence strengthened in 2019, and confirmed via astrometry in 2020. The 2020 study estimates an inclination of 31° for the outer planet, while a 2022 study estimates an inclination of 57.5°.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥3.259+0.377 −0.409 MJ |
1.022+0.055 −0.062 |
317.6+1.6 −1.4 |
0.280+0.036 −0.041 |
— | — |
| c | 19.821+2.430 −2.575 MJ |
6.805+0.536 −0.468 |
5429.9+450.3 −286.0 |
0.164+0.057 −0.056 |
57.478+4.552 −3.652° |
— |
References
- ^ "HD 113337". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 October 2020.
- ^ ПЛАНЕТНЫЕ СИСТЕМЫ HD 113337 HIP 63584 HR 4934
- ^ Janson, Markus; Hormuth, Felix; Bergfors, Carolina; Brandner, Wolfgang; Hippler, Stefan; Daemgen, Sebastian; Kudryavtseva, Natalia; Schmalzl, Eva; Schnupp, Carolin; Henning, Thomas (2012), "The AstraLux Large M-dwarf Multiplicity Survey", The Astrophysical Journal, 754 (1): 44, arXiv:1205.4718, Bibcode:2012ApJ...754...44J, doi:10.1088/0004-637X/754/1/44, S2CID 118475425
- ^ 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.
- ^ Borgniet, Simon; Perraut, K.; Su, K.; Bonnefoy, M.; Delorme, Philippe; Lagrange, Anne-Marie; Bailey, V.; Buenzli, E.; Defrère, D.; Henning, T.; Hinz, P.; Leisenring, J.; Meunier, Nadège; Mourard, D.; Nardetto, N.; Skemer, A. (2020), "Constraints on HD 113337 fundamental parameters and planetary system. Combining long-base visible interferometry, disc imaging, and high-contrast imaging", Astronomy & Astrophysics, A44: 627, arXiv:1905.11156, doi:10.1051/0004-6361/201935494, S2CID 166228639
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- ^ Xuan, Jerry W.; Kennedy, Grant M.; Wyatt, Mark C.; Yelverton, Ben (2020), "Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529", Monthly Notices of the Royal Astronomical Society, 499 (4): 5059–5074, arXiv:2010.02961, Bibcode:2020MNRAS.499.5059X, doi:10.1093/mnras/staa3155, S2CID 222177269
- ^ Yelverton, Ben; Kennedy, Grant M.; Su, Kate Y L.; Wyatt, Mark C. (2019), "A statistically significant lack of debris discs in medium separation binary systems", Monthly Notices of the Royal Astronomical Society, 488 (3): 3588–3606, arXiv:1907.04800, Bibcode:2019MNRAS.488.3588Y, doi:10.1093/mnras/stz1927, S2CID 195874349
- ^ Ginski, C.; Mugrauer, M.; Seeliger, M.; Buder, S.; Errmann, R.; Avenhaus, H.; Mouillet, D.; Maire, A.-L.; Raetz, S. (2016), "A lucky imaging multiplicity study of exoplanet host stars II", Monthly Notices of the Royal Astronomical Society, 457 (2): 2173–2191, arXiv:1601.01524, Bibcode:2016MNRAS.457.2173G, doi:10.1093/mnras/stw049, S2CID 53626523
- ^ Rhee, Joseph H.; Song, Inseok; Zuckerman, B.; McElwain, Michael (2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal, 660 (2): 1556–1571, arXiv:astro-ph/0609555, Bibcode:2007ApJ...660.1556R, doi:10.1086/509912, S2CID 11879505
- ^ Borgniet, Simon; Boisse, Isabelle; Lagrange, Anne-Marie; Bouchy, François; Arnold, Luc; Díaz, Rodrigo F.; Galland, Franck; Delorme, Philippe; Hébrard, Guillaume; Santerne, Alexandre; Ehrenreich, David; Ségransan, Damien; Bonfils, Xavier; Delfosse, Xavier; Santos, Nuno C.; Forveille, Thierry; Moutou, Claire; Udry, Stéphane; Eggenberger, Anne; Pepe, Francesco; Astudillo-Defru, Nicola; Montagnier, Guillaume (2013), "Extrasolar planets and brown dwarfs around A--F type stars. VIII. A giant planet orbiting the young star HD113337", Astronomy & Astrophysics, 561: A65, arXiv:1310.1994, doi:10.1051/0004-6361/201321783, S2CID 118538542
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- ^ 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.
