HD 179949 b
| Exoplanet | List of exoplanets | |
|---|---|---|
| Parent star | ||
| Star | HD 179949 | |
| Constellation | Sagittarius | |
| Right ascension | (α) | 19h 15m 33.23s |
| Declination | (δ) | -24° 10' 45.67" |
| Distance | 88.18 ly (27.05 pc) | |
| Spectral type | F8V | |
| Orbital elements | ||
| Semi-major axis | (a) | 0.0443±0.0026 AU |
| Eccentricity | (e) | 0.022±0.015 |
| Orbital period | (P) | 3.092514±0.000032 d |
| Inclination | (i) | 67.7±4.3° |
| Argument of periastron |
(ω) | 192° |
| Time of periastron | (T0) | 2,451,002.32±0.44 JD |
| Semi-amplitude | (K) | 112.6±1.8 m/s |
| Physical characteristics | ||
| Mass | (m) | 0.98±0.077[1] MJ |
| Discovery information | ||
| Discovery date | Dec 16, 2000 | |
| Discoverer(s) | Tinney, Butler, Marcy et al. | |
| Discovery method | Radial velocity | |
| Discovery site | Anglo-Australian Observatory | |
| Discovery status | Published | |
HD 179949 b is an extrasolar planet discovered by the Anglo-Australian Planet Search at the Anglo-Australian Observatory, which orbits the star HD 179949. The planet is a so-called "hot Jupiter", a Jupiter-mass planet orbiting very close to its parent star. In this case, orbital distance is almost one-tenth that of Mercury from the Sun. One orbital revolution lasts only about 3 days.[2][3]
Its magnetic field induces a bright spot on its star at 30 degrees latitude, which rotates at 87 degrees inclination. If the planet orbited at 83-97 degrees, then its transit would be visible from Earth. The angle of inclination is therefore 83 degrees or less, but not much less; and its mass is constrained to not much more than 0.923±0.077. The star is not tidally locked to the planet.[4]
Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be 1533 K. This is, like Tau Boötis b, hotter than the predicted temperature of HD 209458 b (1392K), and close to that of HD 149026 b, before they were measured.
Searches for water in the planet's atmosphere have been inconclusive, as have attempts to determine whether titanium and vanadium oxides are present.[5]
HD 179949 b is a candidate for "near-infrared characterisation.... with the VLTI Spectro-Imager".[6]
References
- ↑ http://arxiv.org/pdf/1404.3769v1.pdf
- ↑ Tinney, C. G.; et al. (2001). "First Results from the Anglo-Australian Planet Search: A Brown Dwarf Candidate and a 51 Peglike Planet". The Astrophysical Journal. 551 (1): 507–511. arXiv:astro-ph/0012204
. Bibcode:2001ApJ...551..507T. doi:10.1086/320097. - ↑ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
- ↑ Shkolnik and Walker; Walker, G. A. H.; Bohlender, D. A. (2003). "Evidence for Planet-induced Chromospheric Activity on HD 179949". The Astrophysical Journal. 597 (2): 1092–1096. Bibcode:2003ApJ...597.1092S. doi:10.1086/378583.
- ↑ J. R. Barnes; Barman; Jones; Leigh; Cameron; Barber; Pinfield; et al. (3 Oct 2008). "HD 179949b: a close orbiting extrasolar giant planet with a stratosphere?". Monthly Notices of the Royal Astronomical Society. 390 (3): 1258. arXiv:0806.0298. Bibcode:2008MNRAS.390.1258B. doi:10.1111/j.1365-2966.2008.13831.x.
- ↑ Renard, S.; Absil, O.; Berger, J.-P.; Bonfils, X.; Forveille, T.; Malbet, F. (2008). "Prospects for near-infrared characterisation of hot Jupiters with the VLTI Spectro-Imager (VSI)". Optical and Infrared Interferometry. Optical and Infrared Interferometry. Edited by Schöller. Optical and Infrared Interferometry. 7013. pp. 70132Z. arXiv:0807.3014. Bibcode:2008SPIE.7013E..2ZR. doi:10.1117/12.790494.
External links
Coordinates: 
19h 15m 33.23s, −24° 10′ 45.67″