HD 60532
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 07h 34m 03.181s[1] |
| Declination | –22° 17′ 45.84″[1] |
| Apparent magnitude (V) | 4.450[2] |
| Characteristics | |
| Spectral type | F6 IV-V[3] |
| U−B color index | +0.07[4] |
| B−V color index | +0.51[4] |
| Astrometry | |
| Radial velocity (Rv) | 61.042±0.0004[5] km/s |
| Proper motion (μ) | RA: –40.180 mas/yr[1] Dec.: 46.791 mas/yr[1] |
| Parallax (π) | 38.1379 ± 0.1087 mas[1] |
| Distance | 85.5 ± 0.2 ly (26.22 ± 0.07 pc) |
| Absolute magnitude (MV) | 2.40[2] |
| Details | |
| Mass | 1.44+0.03 −0.1[6] M☉ |
| Radius | 2.66±0.03[7] R☉ |
| Luminosity | 9.3±0.1[7] L☉ |
| Surface gravity (log g) | 3.75±0.02[7] cgs |
| Temperature | 6,095[6] K |
| Metallicity [Fe/H] | –0.42[6] dex |
| Rotational velocity (v sin i) | 8[6] km/s |
| Age | 2.7±0.1[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| ARICNS | data |
HD 60532 is a star with two orbiting exoplanets in the southern constellation of Puppis. The designation HD 60532 takes its name from the Henry Draper Catalogue. The system is located at a distance of 85.5 light years from the Sun, and is drifting further away with a radial velocity of 61 km/s.[5] At that distance, the star has an apparent visual magnitude of 4.45,[2] which is bright enough to be faintly visible to the naked eye. The motion of this system through space brought it within 10.3 light-years of the Sun some 408,600 years ago.[11]
The spectrum of this star shows blended features of an F-type main-sequence star and an evolving subgiant star, with a corresponding stellar classification of F6 IV-V.[3] It is an estimated 2.7 billion years old with a projected rotational velocity of 8 km/s and a low level of magnetic activity in its chromosphere.[6] The star has 1.44[6] times the mass of the Sun and 2.66 times the Sun's radius.[7] The abundance of iron, a measure of the star's metallicity, is a scant 38% of solar.[6] HD 60532 is radiating 9.3[7] times the luminosity of the Sun from its photosphere at an effective temperature of 6,095 K.[6]
Planetary system
[edit]In September 2008, two Jupiter-like planets were found orbiting the star.[6] The orbital periods of these two planets appear to be in 3:1 resonance.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.06±0.08 MJ | 0.77±0.02 | 201.9±0.3 | 0.26±0.02 | — | — |
| c | ≥2.51±0.16 MJ | 1.60±0.04 | 600.1±2.4 | 0.03±0.02 | — | — |
See also
[edit]References
[edit]- ^ a b c d 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 Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ a b Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ a b Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ a b 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.
- ^ a b c d e f g h i j Desort, M.; et al. (2008), "Extrasolar planets and brown dwarfs around A-F type stars V. A planetary system found with HARPS around the F6IV-V star HD 60532", Astronomy and Astrophysics, 491 (3): 883–888, arXiv:0809.3862, Bibcode:2008A&A...491..883D, doi:10.1051/0004-6361:200810241, S2CID 14562319.
- ^ a b c d e Bonfanti, A.; et al. (2016), "Age consistency between exoplanet hosts and field stars", Astronomy & Astrophysics, 585: 14, arXiv:1511.01744, Bibcode:2016A&A...585A...5B, doi:10.1051/0004-6361/201527297, S2CID 53971692, A5.
- ^ "HD 60532". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-01-06.
- ^ Gould, Benjamin Apthorp (1879), Uranometria Argentina: brightness and position of every fixed star, down to the seventh magnitude, within one hundred degrees of the South Pole, vol. 1, Observatorio Nacional Argentino, p. 172.
- ^ Gould, Benjamin Apthorp; Pilcher, Frederick, Uranometria Argentina, Revised, archived from the original on 2012-02-27, retrieved 2011-12-08.
- ^ Bailer-Jones, C.A.L.; Rybizki, J.; Andrae, R.; Fouesnea, M. (2018), "New stellar encounters discovered in the second Gaia data release", Astronomy & Astrophysics, 616: A37, arXiv:1805.07581, Bibcode:2018A&A...616A..37B, doi:10.1051/0004-6361/201833456, S2CID 56269929.
- ^ Laskar, J.; Correia, A. C. M. (2009), "HD60532, a planetary system in a 3:1 mean motion resonance", Astronomy & Astrophysics Letters, 496 (2): L5–L8, arXiv:0902.0667, Bibcode:2009A&A...496L...5L, doi:10.1051/0004-6361/200911689, S2CID 17793870.
- ^ Borgniet, S.; et al. (2017), "Extrasolar planets and brown dwarfs around AF-type stars. IX. The HARPS southern sample", Astronomy and Astrophysics, 599, A57, arXiv:1608.08257, Bibcode:2017A&A...599A..57B, doi:10.1051/0004-6361/201628805, S2CID 118723455.
External links
[edit]- "HD 60532". Exoplanets. Archived from the original on 2009-11-24. Retrieved 2008-11-09.
