WASP-32
| Observation data Epoch J2000 Equinox | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 15m 50.80778s[1] |
| Declination | 01° 12′ 01.5868″[1] |
| Apparent magnitude (V) | 11.26[2] |
| Characteristics | |
| Evolutionary stage | main sequence star |
| Spectral type | G0V |
| B−V color index | -0.2 |
| J−H color index | 0.005 |
| J−K color index | 0.342 |
| Astrometry | |
| Radial velocity (Rv) | 18.41±0.83[3] km/s |
| Proper motion (μ) | RA: 1.896±0.09[1] mas/yr Dec.: 16.589±0.062[1] mas/yr |
| Parallax (π) | 3.5949 ± 0.0431 mas[1] |
| Distance | 910 ± 10 ly (278 ± 3 pc) |
| Details | |
| Mass | 1.10±0.03[4] M☉ |
| Radius | 1.11±0.05[4] R☉ |
| Luminosity | 1.5 L☉ |
| Surface gravity (log g) | 4.39±0.03[4] cgs |
| Temperature | 6100±100[4] K |
| Metallicity [Fe/H] | −0.13±0.10[4] dex |
| Rotational velocity (v sin i) | 4.8±0.8[4] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
WASP-32 (also known as TYC 2-1155-1) is a yellow main-sequence star in the constellation of Pisces. The star was given the formal name Parumleo in January 2020, Latin for small lion and referencing the national animal of Singapore.[5]
Star characteristics
The WASP-32 star is relatively depleted of lithium, which is common for massive stars hosting hot Jupiter planets.[4]
Planetary system
The "hot Jupiter" class planet WASP-32 b, later named Viculus, was discovered around WASP-32 in 2010.[4] It was found to orbit the parent star in prograde direction in 2014.[6]
The follow-up study utilizing transit timing variation analysis, have failed to find any, therefore have excluded existence of other massive planets around WASP-32 as in 2015.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Viculus) | 3.6±0.07 MJ | 0.0394±0.0003 | 2.71865±0.00008 | 0.018±0.0065 | 85.3±0.5° | 1.18±0.07 RJ |
References
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- ^ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
- ^ "WASP-32". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-05-09.
- ^ a b c d e f g h Maxted, P. F. L.; Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Hellier, C.; Queloz, D.; Smalley, B.; Triaud, A. H. M. J.; West, R. G.; Enoch, R.; Lister, T. A.; Pepe, F.; Pollacco, D. L.; Ségransan, D.; Skillen, I.; Udry, S. (2010). "WASP-32b: A Transiting Hot Jupiter Planet Orbiting a Lithium-Poor, Solar-Type Star". Publications of the Astronomical Society of the Pacific. 122 (898): 1465–1470. arXiv:1010.1742. Bibcode:2010PASP..122.1465M. doi:10.1086/657658. S2CID 55625415.
- ^ A star and its orbiting planet now bear names with Singapore connection
- ^ Brothwell, R. D.; Watson, C. A.; Hébrard, G.; Triaud, A. H. M. J.; Cegla, H. M.; Santerne, A.; Hébrard, E.; Anderson, D. R.; Pollacco, D.; Simpson, E. K.; Bouchy, F.; Brown, D. J. A.; Chew, Y. Gómez Maqueo; Cameron, A. Collier; Armstrong, D. J.; Barros, S. C. C.; Bento, J.; Bochinski, J.; Burwitz, V.; Busuttil, R.; Delrez, L.; Doyle, A. P.; Faedi, F.; Fumel, A.; Gillon, M.; Haswell, C. A.; Hellier, C.; Jehin, E.; Kolb, U.; et al. (2014). "A window on exoplanet dynamical histories: Rossiter–Mc Laughlin observations of WASP-13b and WASP-32b". Monthly Notices of the Royal Astronomical Society. 440 (4): 3392–3401. arXiv:1403.4095. Bibcode:2014MNRAS.440.3392B. doi:10.1093/mnras/stu520. S2CID 118435056.
- ^ Lei-Lei Sun, Sheng-Hong Gu, Xiao-Bin Wang at al., "Long-term transit timing monitoring and homogenous study of WASP-32", 2015
- ^ Planet WASP-32 b
