Astronomy:HR 2562 B
| Discovery | |
|---|---|
| Discovered by | Q. Konopacky et al.[1] |
| Discovery date | 2016 |
| Direct imaging | |
| Orbital characteristics[3] | |
| 22.2+3.8 −2.9 AU | |
| Eccentricity | 0.34+0.23 −0.18 |
| Orbital period | 71.5+35.7 −23.2[2] yr |
| Inclination | 86.7+0.5 −0.7° |
| Longitude of ascending node | 119.5+0.3 −0.7 |
| 37+32 −24 | |
| Star | HR 2562 |
| Physical characteristics | |
| Mean radius | 0.89+0.14 −0.27[4] RJ |
| Mass | < 22[3] MJ |
| log(g) = 4.70 ± 0.32[1] m/s² | |
| Physics | 1200 ± 100 K[1] |
HR 2562 B is a substellar companion orbiting the star HR 2562. Discovered in 2016 by a team led by Quinn M. Konopacky by direct imaging, HR 2562 B orbits within the inner edge of HR 2562's circumstellar disc—as of April 2023, it is one of only two known brown dwarfs to do so.[2] Separated by roughly 20 Astronomy:astronomical unit|astronomical units (3.0×109 km) from its primary companion, HR 2562 B has drawn interest for its potential dynamical interactions with the outer circumstellar disc.
Discovery
HR 2562 B was discovered using the Gemini Planet Imager (GPI), which first observed the star HR 2562 in January 2016. In the initial data set, Konopacky and collaborators identified a candidate companion object. As a result, followup observations were conducted within the following month in the infrared K1-, K2-, and J-bands. Within the processed data set, HR 2562 B was confirmed to share a common proper motion with HR 2562, with Konopacky and collaborators announcing its discovery in a paper published on 14 September 2016.[1]
Host star
![Image of the disk around HR 2562 with the REASONS survey[5]](/wiki/File:The_74_exocomet_belts_imaged_by_ALMA%E2%80%99s_REASONS_survey,_showing_belts_of_all_shapes,_sizes_and_ages_(REASONS_comboplot_full_nonames).jpg)
HR 2562 B's parent star, HR 2562 (alternatively designated HD 50571 or HIP 32775), has a mass of 1.368±0.018 M☉ and a radius of 1.334±0.027 R☉. With an estimated effective temperature of 6597 ± 81K, it is a main-sequence star with the spectral type F5V. It is located 110.92 ± 0.16 light-years (34.007 ± 0.048 pc) from the Sun in the constellation Pictor.[6] HR 2562 is not known to belong to a moving group or stellar cluster.[4][7]
As with many mid F-type stars, the age of HR 2562 is poorly constrained. Between 1999 and 2011, estimates from various teams of astronomers determined ages ranging from roughly 300 Myr to 1.6 Gyr. In 2018, a team of astronomers led by D. Mesa derived an age of 450+300
−250 Myr using measurements of the star's lithium-temperature relationship.[7]
Properties
Orbital properties
Initial observations of HR 2562 B by Konopacky and collaborators yielded a separation of 20.3 ± 0.3 AU (3.037×109 ± 45,000,000 km), placing it interior to and coplanar with the inner edge of HR 2562's observed debris disc.[1] Further observations of HR 2562 B by the Atacama Large Millimeter Array (ALMA) supported this, yielding a semi-major axis of 19.0+5.7
−4.4 AU, an orbital period of 71.5+35.7
−23.2 yr, and an orbital eccentricity of 0.63+0.32
−0.23. With a probable orbital inclination of 82.8+2.0
−12.5°, HR 2562 B's misalignment angle with the debris disc is either 7+17
−4° or 15+18
−5°. However, the limited coverage of observations still leaves a wide range of possible orbits; both low-eccentricity, coplanar orbits and high-eccentricity, misaligned orbits would be consistent with observation data. However, a highly misaligned orbit would significantly perturb the disc, suggesting that a low-eccentricity, coplanar solutions are likelier.[2] A 2025 study using astrometry and radial velocity refined the orbital elements, finding a separation of 22.2 AU, a significantly lower eccentricity of 0.34, and an inclination of 86.7°, which implies a planet-disk inclination of 3.7±0.3°.[3]
Any additional companions around HR 2562 with a mass on the order of 10 MJ should be visible at separations larger than 10 AU, and any companion a few times more massive than Jupiter should be visible to SPHERE's infrared dual-band spectrograph (IRDIS) instrument—thus placing mass restrictions on any additional companions.[7]
Physical properties
HR 2562 B's exact mass is unknown. The brown dwarf was estimated to be 29 ± 15 MJ in 2021.[4] However, subsequent observations placed an upper mass limit of 18.5 MJ[2] and later 22 MJ.[3] Its luminosity is about solar luminosity.[1][note 1] Its spectral type is L7±3.[1]
See also
- PZ Telescopii B, another substellar object with mass slightly below 30 MJ
Notes
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Konopacky, Quinn M.; Rameau, Julien; Duchêne, Gaspard; Filippazzo, Joseph C.; Godfrey, Paige A. Giorla; Marois, Christian; Nielsen, Eric L.; Pueyo, Laurent et al. (2016). "Discovery of a Substellar Companion to the Nearby Debris Disk Host HR 2562" (in en). The Astrophysical Journal Letters 829 (1): L4. doi:10.3847/2041-8205/829/1/L4. ISSN 2041-8205. Bibcode: 2016ApJ...829L...4K.
- ↑ 2.0 2.1 2.2 2.3 Zhang, Stella Yimao (28 April 2023). "Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System". The Astronomical Journal 165 (5): 219. doi:10.3847/1538-3881/acbafb. Bibcode: 2023AJ....165..219Z.
- ↑ 3.0 3.1 3.2 3.3 Roberts, Jonathan; Thompson, William; Wang, Jason J.; Blunt, Sarah; Balmer, William O.; Bourdarot, Guillaume; Bowler, Brendan P.; Chauvin, Gael; Eisenhauer, Frank; Henning, Thomas K.; Kammerer, Jens; Kiefer, Flavien; Kenworthy, Matthew A.; Kervella, Pierre; Lacour, Sylvestre; Lagrange, A. -M.; Nielsen, Eric L.; Pueyo, Laurent; Rickman, Emily; Sipilä, Olli; Spezzano, Silvia; Stolker, Tomas; Zurlo, Alice (2025). "New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities". arXiv:2509.14321 [astro-ph.EP].
- ↑ 4.0 4.1 4.2 Sutlieff, Ben J.; Bohn, Alexander J.; Birkby, Jayne L.; Kenworthy, Matthew A.; Morzinski, Katie M.; Doelman, David S.; Males, Jared R.; Snik, Frans et al. (2021). "High-contrast observations of brown dwarf companion HR 2562 B with the vector Apodizing Phase Plate coronagraph". Monthly Notices of the Royal Astronomical Society 506 (3): 3224–3238. doi:10.1093/mnras/stab1893. Bibcode: 2021MNRAS.506.3224S.
- ↑ Matrà, L.; Marino, S.; Wilner, D. J.; Kennedy, G. M.; Booth, M.; Krivov, A. V.; Williams, J. P.; Hughes, A. M. et al. (2025-01-15). "REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths". Astronomy and Astrophysics 693. doi:10.1051/0004-6361/202451397. Bibcode: 2025A&A...693A.151M.
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R Constellation record for this object at VizieR.
- ↑ 7.0 7.1 7.2 Mesa, D. (4 May 2018). "New spectro-photometric characterization of the substellar object HR 2562 B using SPHERE". Astronomy & Astrophysics 612: A92. doi:10.1051/0004-6361/201731649. Bibcode: 2018A&A...612A..92M.
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