HD 179949 / Gumala
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 19h 15m 33.22990s[1]
Declination −24° 10′ 45.6668″[1]
Apparent magnitude (V) 6.25[2]
Characteristics
Spectral type F8 V[3]
B−V color index 0.548±0.009[2]
Astrometry
Radial velocity (Rv)−24.56±0.08[2] km/s
Proper motion (μ) RA: +117.97[1] mas/yr
Dec.: −101.67[1] mas/yr
Parallax (π)36.30 ± 0.70 mas[1]
Distance90 ± 2 ly
(27.5 ± 0.5 pc)
Absolute magnitude (MV)4.05[2]
Details[4]
Mass1.23±0.01 M☉
Radius1.2±0.01 R☉
Luminosity1.95±0.01 L☉
Surface gravity (log g)4.36±0.01 cgs
Temperature6,220±28 K
Metallicity [Fe/H]+0.21[5] dex
Rotational velocity (v sin i)6.84 km/s
Age1.20±0.60 Gyr
Other designations
13 Sgr, V5652 Sgr, CD−24° 15161, GJ 749, HD 179949, HIP 94645, HR 7291, SAO 187883[6]
Database references
SIMBADdata

HD 179949 is a 6th magnitude star in the constellation of Sagittarius. It is a yellow-white dwarf (spectral class F8 V), a type of star hotter and more luminous than the Sun. The star is located about 90 light years from Earth and might be visible under exceptionally good conditions to an experienced observer without technical aid; usually binoculars are needed.

The star HD 179949 is named Gumala. The name was selected in the NameExoWorlds campaign by Brunei,[7] during the 100th anniversary of the IAU. Gumala is a Malay word, which means a magic bezoar stone found in snakes, dragons, etc.[8][9]

Properties

This is an F-type main-sequence star classified with a spectral type of F8V.[3] It has an estimated mass of 1.23 times the solar mass and a radius of 1.20 times the solar radius.[4] Its photosphere is shining with 1.95 times the solar luminosity at an effective temperature of 6,220 K.[4] Its metallicity, the abundance of elements other than hydrogen and helium, is high, with 162% the solar iron abundance, following the trend that stars with giant planets are more metal-rich.[10]

With an estimated age of 1.2 billion years,[4] HD 179949 is a chromospherically active star and has a complex magnetic field with a maximum strength of 10 G. Like the Sun, this star has differential rotation, with the equatorial region having a faster rotation period, of 7.62 ± 0.07 days, compared to a rotation period of 10.3 ± 0.8 days in the poles.[11] The star's projected rotational velocity is 7.0 km/s,[12] corresponding to an inclination angle of about 60°.[11] HD 179949 has been classified as a BY Draconis variable, which varies in brightness due to rotational modulation of spots on the surface.[13]

Monitoring of the star's spectral lines suggested a possible correlation between the star's chromospheric activity and the orbital period of its planet HD 179949 b. Later observations showed that this correlation is not present, with the star's activity being in synchrony with the star's rotation, instead of the exoplanet's orbit.[11][14] By 2022, stellar X-ray flares correlation with the planetary orbit was not detected too.[15]

Planetary system

The discovery of an extrasolar planet orbiting HD 179949 with a period of only 3.1 days was published in 2001. It was detected with the radial velocity method from observations of the star with the UCLES spectrograph, in the Anglo-Australian Telescope, as part of the Anglo-Australian Planet Search.[16] With a minimum mass of 92% of the mass of Jupiter, it is a hot Jupiter, orbiting the star at a distance of only 0.04 AU. Its orbit is nearly circular, with a best fit orbital eccentricity of 0.022 ± 0.015.[17] Planets close to their stars have high chances of transit, but photometric observations of HD 179949 ruled out this possibility.[16]

Infrared observations of HD 179949 with the Spitzer Space Telescope detected 0.14% variations in the system's brightness in phase with the orbital period of the planet, indicating large luminosity variation between the illuminated side and the dark side of the planet, implying that less than 21% of the incident stellar energy is transferred to the dark side.[18] In 2014, infrared observations of the system with the CRIRES instrument, at the Very Large Telescope, directly detected the thermal spectrum of the planet, revealing absorption features of carbon monoxide and water vapor in its atmosphere. The radial velocity of the planet has variations of 142.8 ± 3.4 km/s due to orbital motion, which allowed the calculation of a real mass of 0.98 ± 0.04 Jupiter masses and an orbital inclination of 67.7 ± 4.3 degrees.[19]

The HD 179949 planetary system[17][19]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b / Mastika 0.98 ± 0.004 MJ 0.0443 ± 0.0026 3.092514 ± 0.000032 0.022 ± 0.015 67.7±4.3° —

References

  1. ^ a b c d e van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c d Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ a b Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  4. ^ a b c d Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
  5. ^ Delgado Mena, E.; et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics, 576: A69, arXiv:1412.4618, Bibcode:2015A&A...576A..69D, doi:10.1051/0004-6361/201425433, S2CID 56051637, A69.
  6. ^ "HD 179949". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-28.
  7. ^ "NameExoWorlds Brunei – Bruneiastronomy.org". Retrieved 2020-10-11.
  8. ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  9. ^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
  10. ^ Sousa, S.G.; et al. (August 2008). "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes". Astronomy and Astrophysics. 487 (1): 373–381. arXiv:0805.4826. Bibcode:2008A&A...487..373S. doi:10.1051/0004-6361:200809698. S2CID 18173201.
  11. ^ a b c Fares, R.; et al. (June 2012). "Magnetic field, differential rotation and activity of the hot-Jupiter-hosting star HD 179949". Monthly Notices of the Royal Astronomical Society. 423 (2): 1006–1017. arXiv:1202.4472. Bibcode:2012MNRAS.423.1006F. doi:10.1111/j.1365-2966.2012.20780.x. S2CID 118475648.
  12. ^ Valenti, J.A.; Fischer, D.A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500.
  13. ^ Samus, N.N.; Durlevich, O.V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Bibcode:2009yCat....102025S.
  14. ^ Scandariato, G.; et al. (April 2013). "A coordinated optical and X-ray spectroscopic campaign on HD 179949: searching for planet-induced chromospheric and coronal activity". Astronomy & Astrophysics. 552: A7. arXiv:1301.7748. Bibcode:2013A&A...552A...7S. doi:10.1051/0004-6361/201219875. S2CID 53354621. A7.
  15. ^ Acharya, Anshuman; Kashyap, Vinay L.; Saar, Steven H.; Kulinder Pal Singh; Cuntz, Manfred (2022), X-ray Activity on the Star-Planet Interaction Candidate HD 179949, arXiv:2211.01011
  16. ^ a b 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. hdl:2299/138. S2CID 7192024.
  17. ^ a b 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. hdl:2299/1103. S2CID 119067572.
  18. ^ Cowan, N.B.; Agol, E.; Charbonneau, D. (August 2007). "Hot nights on extrasolar planets: mid-infrared phase variations of hot Jupiters". Monthly Notices of the Royal Astronomical Society. 379 (2): 641–646. arXiv:0705.1189. Bibcode:2007MNRAS.379..641C. doi:10.1111/j.1365-2966.2007.11897.x. S2CID 16662531.
  19. ^ a b Brogi, M.; de Kok, R.J.; Birkby, J.L.; Schwarz, H.; Snellen, I.A.G. (May 2014). "Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b". Astronomy & Astrophysics. 565: A124. arXiv:1404.3769. Bibcode:2014A&A...565A.124B. doi:10.1051/0004-6361/201423537. S2CID 56450007. A124.

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