Astronomy:WASP-48
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 24m 38.9616s[1] |
| Declination | +55° 28′ 23.3317″[1] |
| Apparent magnitude (V) | 11.65±0.14 |
| Characteristics | |
| Spectral type | G0IV |
| Astrometry | |
| Radial velocity (Rv) | -19.740 km/s |
| Proper motion (μ) | RA: 6.141 mas/yr Dec.: -27.969 mas/yr |
| Parallax (π) | 2.1732 ± 0.0213[1] mas |
| Distance | 1,500 ± 10 ly (460 ± 5 pc) |
| Details[2] | |
| Mass | 1.19±0.04 M☉ |
| Radius | 1.75±0.07 R☉ |
| Surface gravity (log g) | 4.03±0.03 cgs |
| Temperature | 5920±150 K |
| Metallicity | −0.12±0.12 |
| Rotational velocity (v sin i) | 12.2±0.7 km/s |
| Age | 6+5−4 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WASP-48 is a subgiant star about 1400 light-years away. The star is likely older than Sun and slightly depleted in heavy elements. It shows an infrared excess noise of unknown origin,[3] yet has no detectable ultraviolet emissions associated with the starspot activity.[4] The discrepancy may be due to large interstellar absorption of light in interstellar medium for WASP-48.[5] The measurements are compounded by the emission from eclipsing contact binary NSVS-3071474 projected on sky plane nearby,[6] although no true stellar companions were detected by survey in 2015.[7]
The star is rotating rapidly, being spun up by the tides raised by the giant planet on close orbit.[8]
Planetary system
In 2011 a transiting hot Jupiter planet b was detected.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.98±0.09 MJ | 0.03320±0.00077 | 2.143634±0.000003 | 0 | 80.09+0.69−0.55° | 1.396±0.051 RJ |
References
- ↑ 1.0 1.1 1.2 1.3 WASP-48 -- Star
- ↑ 2.0 2.1 2.2 Enoch, B.; Anderson, D. R.; Barros, S. C. C.; Brown, D. J. A.; Collier Cameron, A.; Faedi, F.; Gillon, M.; Hébrard, G. et al. (2011), WASP-35b, WASP-48b and WASP-51b: Two new planets and an independent discovery of HAT-P-30b, doi:10.1088/0004-6256/142/3/86
- ↑ Sada, Pedro V.; Deming, Drake; Jennings, Donald E.; Jackson, Brian k.; Hamilton, Catrina M.; Fraine, Jonathan; Peterson, Steven W.; Haase, Flynn et al. (2012), "Extrasolar Planet Transits Observed at Kitt Peak National Observatory", Publications of the Astronomical Society of the Pacific 124 (913): 212–229, doi:10.1086/665043, Bibcode: 2012PASP..124..212S
- ↑ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal 766 (1): 9, doi:10.1088/0004-637X/766/1/9, Bibcode: 2013ApJ...766....9S
- ↑ Fossati, L.; Marcelja, S. E.; Staab, D.; Cubillos, P. E.; France, K.; Haswell, C. A.; Ingrassia, S.; Jenkins, J. S. et al. (2017), "The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies", Astronomy & Astrophysics 601: A104, doi:10.1051/0004-6361/201630339, Bibcode: 2017A&A...601A.104F
- ↑ 6.0 6.1 Ciceri, S.; Mancini, L.; Southworth, J.; Bruni, I.; Nikolov, N.; d'Ago, G.; Schröder, T.; Bozza, V. et al. (2015), "Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry", Astronomy & Astrophysics 577: A54, doi:10.1051/0004-6361/201425449, Bibcode: 2015A&A...577A..54C
- ↑ Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics 575: A23, doi:10.1051/0004-6361/201424091, Bibcode: 2015A&A...575A..23W
- ↑ 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, doi:10.1093/mnras/stu950, Bibcode: 2014MNRAS.442.1844B
Coordinates: 
19h 24m 38.9616s, +55° 28′ 23.3317″
 |  |
