WASP-37
| Observation data Epoch J2000 Equinox | |
|---|---|
| Constellation | Virgo |
| Right ascension | 14h 47m 46.5618s |
| Declination | 01° 03′ 53.8024″ |
| Apparent magnitude (V) | 12.704 |
| Characteristics | |
| Evolutionary stage | main sequence star |
| Spectral type | G2V |
| U−B color index | 0.022 |
| B−V color index | 0.628 |
| V−R color index | 0.337 |
| J−H color index | 0.378 |
| J−K color index | 0.406 |
| Astrometry | |
| Radial velocity (Rv) | 7.927±0.0042 km/s |
| Proper motion (μ) | RA: -28.082±0.069 mas/yr Dec.: 18.018±0.062 mas/yr |
| Parallax (π) | 2.5183 ± 0.0493 mas |
| Distance | 1,300 ± 30 ly (397 ± 8 pc) |
| Details[1][2] | |
| Mass | 0.925±0.12 M☉ |
| Radius | 1.003±0.053 R☉ |
| Surface gravity (log g) | 4.386 cgs |
| Temperature | 5800±150 K |
| Metallicity [Fe/H] | -0.40±0.12 dex |
| Rotational velocity (v sin i) | 2.4±1.6 km/s |
| Age | 10.31+4.01 −2.55 Gyr |
| Other designations | |
WASP-37, DENIS J144746.5+010354, 2MASS J14474655+0103538, Gaia DR2 3652176997218325888[3] | |
| Database references | |
| SIMBAD | data |
WASP-37 is a yellow main sequence star in the constellation of Virgo.
Star characteristics
WASP-37 has a low metallicity of just 40% of solar,[4] and is likely older than Sun.[2] WASP-37 does not have noticeable flare activity.[5]
Planetary system
The "Hot Jupiter" class planet WASP-37b was discovered around WASP-37 in 2010.[4] The study in 2018 has found the stability of orbits in habitable zone of WASP-37 is not significantly affected by WASP-37b planet.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.79±0.17 MJ | 0.045±0.002 | 3.5774807±0.0000019 | 0 | 88.78° | 1.16+0.07 −0.06 RJ |
References
- ^ Maxted, P. F. L.; Koen, C.; Smalley, B. (2011). "UBV(RI)C photometry of transiting planet hosting stars". Monthly Notices of the Royal Astronomical Society. 418 (2): 1039–1042. arXiv:1108.0349. Bibcode:2011MNRAS.418.1039M. doi:10.1111/j.1365-2966.2011.19554.x. S2CID 117056033.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b Brown, D. J. A. (2014). "Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?". Monthly Notices of the Royal Astronomical Society. 442 (2): 1844–1862. arXiv:1406.4402. Bibcode:2014MNRAS.442.1844B. doi:10.1093/mnras/stu950. S2CID 56052792.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ WASP-37 -- Star
- ^ a b c Simpson, E. K.; Faedi, F.; Barros, S. C. C.; Brown, D. J. A.; Cameron, A. Collier; Hebb, L.; Pollacco, D.; Smalley, B.; Todd, I.; Butters, O. W.; Hébrard, G.; McCormac, J.; Miller, G. R. M.; Santerne, A.; Street, R. A.; Skillen, I.; Triaud, A. H. M. J.; Anderson, D. R.; Bento, J.; Boisse, I.; Bouchy, F.; Enoch, B.; Haswell, C. A.; Hellier, C.; Holmes, S.; Horne, K.; Keenan, F. P.; Lister, T. A.; Maxted, P. F. L.; et al. (2011). "WASP-37b: A 1.8MJEXOPLANET TRANSITING a METAL-POOR STAR". The Astronomical Journal. 141 (1): 8. arXiv:1008.3096. Bibcode:2011AJ....141....8S. doi:10.1088/0004-6256/141/1/8. S2CID 20036137.
- ^ Shkolnik, Evgenya L. (2013). "An Ultraviolet Investigation of Activity on Exoplanet Host Stars". The Astrophysical Journal. 766 (1): 9. arXiv:1301.6192. Bibcode:2013ApJ...766....9S. doi:10.1088/0004-637X/766/1/9. S2CID 118415788.
- ^ a b Georgakarakos, Nikolaos; Eggl, Siegfried; Dobbs-Dixon, Ian (2018). "Giant Planets: Good Neighbors for Habitable Worlds?". The Astrophysical Journal. 856 (2): 155. arXiv:1804.02183. Bibcode:2018ApJ...856..155G. doi:10.3847/1538-4357/aaaf72. S2CID 119522834.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ Mallonn, M.; von Essen, C.; Herrero, E.; Alexoudi, X.; Granzer, T.; Sosa, M.; Strassmeier, K. G.; Bakos, G.; Bayliss, D.; Brahm, R.; Bretton, M.; Campos, F.; Carone, L.; Colón, K. D.; Dale, H. A.; Dragomir, D.; Espinoza, N.; Evans, P.; Garcia, F.; Gu, S.-H.; Guerra, P.; Jongen, Y.; Jordán, A.; Kang, W.; Keles, E.; Kim, T.; Lendl, M.; Molina, D.; Salisbury, M.; et al. (2019). "Ephemeris refinement of 21 hot Jupiter exoplanets with high timing uncertainties". Astronomy & Astrophysics. 622: A81. arXiv:1812.05882. Bibcode:2019A&A...622A..81M. doi:10.1051/0004-6361/201834194. S2CID 92990448.
 | This main-sequence-star-related article is a stub. You can help Wikipedia by expanding it. |