| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Equuleus[1] |
| Right ascension | 21h 06m 39.842s[2] |
| Declination | +03° 48′ 11.23″[2] |
| Apparent magnitude (V) | +6.48[1] |
| Characteristics | |
| Spectral type | G8 IV[3] |
| B−V color index | 0.880±0.009[1] |
| Astrometry | |
| Radial velocity (Rv) | −72.63±0.03[4] km/s |
| Proper motion (μ) | RA: 94.748 mas/yr[2] Dec.: 50.418 mas/yr[2] |
| Parallax (π) | 13.7656 ± 0.0275 mas[2] |
| Distance | 236.9 ± 0.5 ly (72.6 ± 0.1 pc) |
| Absolute magnitude (MV) | 2.19[1] |
| Details | |
| Mass | 1.44±0.09[5] M☉ |
| Radius | 4.30±0.09[5] R☉ |
| Luminosity | 13.758±0.064[6] L☉ |
| Surface gravity (log g) | 3.6±0.1[5] cgs |
| Temperature | 5,164±44[5] K |
| Metallicity [Fe/H] | −0.15±0.04[5] dex |
| Rotational velocity (v sin i) | 2.28±0.5[5] km/s |
| Age | 3.0±0.6[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 200964 is a star with a pair of orbiting exoplanets[5] located in the northern constellation of Equuleus.[1] It has an apparent visual magnitude of +6.48,[1] which puts it at the lower limit of visibility to the naked eye, but binoculars would make it easy to see. Based on parallax measurements, the distance to this system is 238 light years, but it is drifting closer with a heliocentric radial velocity of −72.6 km/s.[4]
This is a G-type subgiant star[5] with a stellar classification of G8 IV.[3] It is a 3.3 billion year old star that has exhausted the supply of hydrogen at its core and has begun to evolve away from the main sequence, where it was an A-type star.[5] The star has 44% more mass than the Sun and is spinning with a projected rotational velocity of 2.3 km/s. The abundance of iron, an indicator of the star's metallicity, is lower than in the Sun. The star has swelled to 4.3 times the radius of the Sun and it is radiating nearly 14 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,164 K.[5]
Planetary system
On July 26, 2010 the California and Carnegie Planet Search team announced the discovery of two planets around HD 200964 along with two planets around 24 Sextantis.[8] The inner planet is nearly twice as massive as Jupiter and takes 614 days to orbit the star in a circular orbit at the average distance of 1.60 AU (240 Gm). The outer planet is 9/10 the mass of Jupiter and takes 825 days to orbit eccentrically around the star at the average distance of 1.95 AU (292 Gm).
Due to the close proximity of the two planets to each other the discoverers only found stable orbits near the 4:3 resonance, meaning that every time the outer planet orbits the star three times, the inner planet orbits the star four times. The two planets are separated by only 0.35 AU. Because of the small separation between the two massive planets, the gravitational tugs between the two planets is nearly 3 million times greater than the gravitational force between Earth and Mars, 700 times larger than that between Earth and the Moon, and 4 times larger than the pull of the Sun on Earth.[8][5] After additional radial velocity measurements were taken stable solutions in the 7:5 and 3:2 mean-motion resonances were found in addition to the 4:3 mean-motion resonance. The 7:5 configuration currently provides the best match to the measurements.[9]
There is evidence of a possible third planet in the system with a period of ~7 days however the three planet model of the system is only slightly better than the two planet model.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.85+0.14 −0.08 MJ |
1.601 ± 0.002 | 613.8+1.3 −1.4 |
0.04+0.04 −0.02 |
— | 0.85 RJ |
| c | ≥0.90+0.12 −0.06 MJ |
1.950+0.008 −0.005 |
825.0+3.1 −5.1 |
0.181+0.024 −0.017 |
— | 0.85 RJ |
See also
References
- 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- 1 2 3 4 5 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.
- 1 2 Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- 1 2 Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
- 1 2 3 4 5 6 7 8 9 10 11 12 Johnson, John Asher; et al. (2011). "Retired A Stars and Their Companions. VI. A Pair of Interacting Exoplanet Pairs Around the Subgiants 24 Sextanis and HD 200964". The Astronomical Journal. 141 (1). 16. arXiv:1007.4552. Bibcode:2011AJ....141...16J. doi:10.1088/0004-6256/141/1/16.
- ↑ Johns, Daniel; et al. (November 2018). "Revised Exoplanet Radii and Habitability Using Gaia Data Release 2". The Astrophysical Journal Supplement Series. 239 (1): 14. arXiv:1808.04533. Bibcode:2018ApJS..239...14J. doi:10.3847/1538-4365/aae5fb. 14.
- ↑ "HD 200964". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-15.
- 1 2 "Astronomers find planets in unusually intimate dance around dying star". Astronomy Magazine. July 29, 2010. Retrieved 2011-01-13.
- 1 2 Rosenthal, M. M.; et al. (2019). "Measuring the Orbital Parameters of Radial Velocity Systems in Mean-motion Resonance: A Case Study of HD 200964". The Astronomical Journal. 158 (4). 136. arXiv:1908.04789. Bibcode:2019AJ....158..136R. doi:10.3847/1538-3881/ab3b02. S2CID 199577752.
- ↑ "Notes for star 24 Sex". Extrasolar Planets Encyclopaedia. Archived from the original on August 4, 2010. Retrieved 2011-01-13.
