Astronomy:HD 179949 b
| Discovery | |
|---|---|
| Discovered by | Tinney et al. |
| Discovery site | Anglo-Australian Observatory |
| Discovery date | Dec 3, 2000[1] |
| Radial velocity | |
| Orbital characteristics | |
| 0.0443 ± 0.0026 AU (6,630,000 ± 390,000 km) | |
| Eccentricity | 0.022±0.015 |
| Orbital period | 3.092514±0.000032 d |
| Inclination | 67.7±4.3 |
| astron|astron|helion}} | 2,451,002.32±0.44 |
| 192 | |
| Semi-amplitude | 112.6±1.8 |
| Star | HD 179949 |
| Physical characteristics | |
| Mass | 0.98±0.077[2] |♃|J}}}}}} |
HD 179949 b, formally named Mastika, 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.[3][4]
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 about 0.92 Jupiter masses |♃|J}}}}}}. The star is not tidally locked to the planet.[5]
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 at first, as have attempts to determine whether titanium and vanadium oxides are present.[6] In the meantime, both carbon monoxide and water have been found in the dayside emission of HD 179949b.[7]
HD 179949 b is a candidate for "near-infrared characterisation.... with the VLTI Spectro-Imager".[8]
The light reflected off planet could not be detected as in 2021, implying HD 179949 b has a low albedo.[9]
The planet HD 179949 b is named Mastika. The name was selected in the NameExoWorlds campaign by Brunei,[10] during the 100th anniversary of the IAU. Mastika is a Malay word, which means a gem, precious stone, jewel or the prettiest, the most beautiful.[11][12]
References
- ↑ Tinney, Chris (2007-09-07). "AAPS Discovered Planets". University of New South Wales. http://newt.phys.unsw.edu.au/~cgt/planet/AAPS%20Planets.html.
- ↑ Brogi, M.; De Kok, R. J.; Birkby, J. L.; Schwarz, H.; Snellen, I. A. G. (2014). "Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 B". Astronomy & Astrophysics 565: A124. doi:10.1051/0004-6361/201423537. Bibcode: 2014A&A...565A.124B.
- ↑ 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. doi:10.1086/320097. Bibcode: 2001ApJ...551..507T.
- ↑ Butler, R. P. et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505–522. doi:10.1086/504701. Bibcode: 2006ApJ...646..505B. http://www.iop.org/EJ/article/0004-637X/646/1/505/64046.html.
- ↑ 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. doi:10.1086/378583. Bibcode: 2003ApJ...597.1092S. http://www.iop.org/EJ/article/0004-637X/597/2/1092/57949.html.
- ↑ J. R. Barnes 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. doi:10.1111/j.1365-2966.2008.13831.x. Bibcode: 2008MNRAS.390.1258B.
- ↑ Brogi, M.; Kok, R. J. de; Birkby, J. L.; Schwarz, H.; Snellen, I. A. G. (2014). "Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b" (in en). Astronomy & Astrophysics 565: A124. doi:10.1051/0004-6361/201423537. ISSN 0004-6361. Bibcode: 2014A&A...565A.124B.
- ↑ Renard, Stéphanie; Absil, Olivier; Berger, Jean-Philippe; Bonfils, Xavier; Forveille, Thierry; Malbet, Fabien (2008). "Prospects for near-infrared characterisation of hot Jupiters with the VLTI Spectro-Imager (VSI)". Proceedings of SPIE. Optical and Infrared Interferometry 7013: 70132Z–70132Z–10. doi:10.1117/12.790494. Bibcode: 2008SPIE.7013E..2ZR. http://orbi.ulg.ac.be/bitstream/2268/30158/1/SPIE_poster.pdf.
- ↑ Bailey, Jeremy; Bott, Kimberly; Cotton, Daniel V.; Kedziora-Chudczer, Lucyna; Zhao, Jinglin; Evensberget, Dag; Marshall, Jonathan P.; Wright, Duncan et al. (2021), "Polarization of hot Jupiter systems: A likely detection of stellar activity and a possible detection of planetary polarization", Monthly Notices of the Royal Astronomical Society 502 (2): 2331–2345, doi:10.1093/mnras/stab172
- ↑ "NameExoWorlds Brunei – Bruneiastronomy.org" (in en-US). https://bruneiastronomy.org/web/nameexoworlds/.
- ↑ "International Astronomical Union | IAU". https://www.iau.org/news/pressreleases/detail/iau1912/.
- ↑ "Approved names" (in en). http://www.nameexoworlds.iau.org/final-results.
External links
Coordinates: 
19h 15m 33.23s, −24° 10′ 45.67″
es:HD 179949#Sistema planetario ru:HD 179949#HD 179949 b
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