HD 47366

Last updated
HD 47366
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Canis Major
Right ascension 06h 37m 40.793s [1]
Declination −12° 59′ 06.42″ [1]
Apparent magnitude  (V)6.12 [2]
Characteristics
Spectral type K1III: [3]
B−V color index 0.977 [3]
Astrometry
Radial velocity (Rv)9.01 [3]  km/s
Proper motion (μ)RA: 10.239  mas/yr [1]
Dec.: −125.836  mas/yr [1]
Parallax (π)11.8263 ± 0.0636  mas [1]
Distance 276 ± 1  ly
(84.6 ± 0.5  pc)
Absolute magnitude  (MV)1.459 [3]
Details
Mass 1.81±0.13 [4]   M☉
Radius 7.30±0.33 [4]   R☉
Luminosity 26.1±1.8 [4]   L☉
Surface gravity (log g)2.60 [3]   cgs
Temperature 4,772 [3]   K
Metallicity [Fe/H]−0.16 [3]   dex
Rotation < 86 [4] d
Rotational velocity (v sin i)4.3±0.8 [4]  km/s
Age 1.61±0.53 [4]   Gyr
Other designations
BD−12° 1566, HD  47366, HIP  31674, HR  2437, SAO  151725 [5]
Database references
SIMBAD data

HD 47366 is the Henry Draper Catalogue designation for a star in the southern constellation of Canis Major. It has an apparent visual magnitude of 6.12, [2] which puts it near the lower limit of stars visible to the naked eye. According to the Bortle scale, it can be viewed from dark rural skies. Parallax measurements performed by the Gaia spacecraft provide a distance estimate of 276 light-years (85 parsecs ). [1]

This is a K-type giant star with a stellar classification of K1III: − the colon suffix indicates some uncertainty in the luminosity classification of III. [3] Spectroscopic analysis of the star was used to derive an estimated mass of about 1.81 times the mass of the Sun. It has an estimated age of 1.6 billion years; old enough at that mass to have evolved off the main sequence. As a giant star, the atmosphere has expanded to 7.3 times the Sun's radius, and it is emitting 26 times the solar luminosity at an effective temperature of 4,772 K. The projected rotational velocity of the star is 4.3 km/s, indicating it is rotating with a period of under 86 days. [4]

In 2016, a team of astronomers reported the detection of a pair of giant planetary companions. Radial velocity measurements indicated gravitational perturbations of the star being caused by orbiting objects. The best fit to the preliminary data suggests two periodicities: one almost exactly a year long like the Earth's periodicity, and a second of around two years. Both objects are predicted to have masses greater than that of the planet Jupiter: their minimum masses are 1.8 and 1.9 Jupiter masses, respectively. Until the inclination of their orbits is known, their actual masses cannot be pinned down more accurately. [4]

The HD 47366 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≥ 1.75+0.20
−0.17  MJ 		1.214+0.030
−0.029		363.3+2.5
−2.4		0.089+0.079
−0.060		——
c≥ 1.86+0.16
−0.15  MJ 		1.853+0.045
−0.045		684.7+5.0
−4.9		0.278+0.069
−0.094		——

Modelling of the orbits of the two planets showed that they are dynamically unstable on the life span of their host star unless they are in a 2:1 mean motion resonance or are on mutually retrograde orbits. [4] In 2019, J. P. Marshall and associates proposed an orbital fit with lower eccentricities that is more stable. The new fit is closer to the 2:1 mean motion resonance. As the host star continues to evolve to a larger radius, it is expected that both planets will undergo orbital decay due to tidal forces and be engulfed. [6]

Related Research Articles

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HD 66428 is a G-type main sequence star located approximately 174 light-years away in the constellation of Monoceros. This star is similar to the Sun with an apparent magnitude of 8.25, an effective temperature of 5705 ± 27 K and a solar luminosity 1.28. Its absolute magnitude is 11.1 while its U-V color index is 0.71. It is considered an inactive star and it is metal-rich . This star has a precise mass of 1.14552 solar masses. This precision comes from the Corot mission that measured asteroseismology.

HD 59686 is a binary star system in the northern constellation of Gemini. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.45. The distance to this system is approximately 292 light years based on parallax, but it is drifting closer with a radial velocity of −34 km/s.

HD 231701 is a yellow-white hued star in the northern constellation of Sagitta, near the southern constellation border with Aquila. With an apparent visual magnitude of 8.97, it is too dim to be viewed with the naked eye, but can be seen with powerful binoculars or a small telescope. Parallax measurements provide a distance estimate of approximately 356 light years from the Sun, but it is drifting closer with a radial velocity of −63 km/s. It is predicted to come as close as 189.5 light-years in 1.345 million years.

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HD 73256 is a variable star in the southern constellation of Pyxis. It has the variable star designation CS Pyxidis. With a baseline apparent visual magnitude of 8.08, it requires binoculars or a small telescope to view. The star is located at a distance of 120 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +30 km/s.

HD 109749 is a binary star about 206 light years away in the constellation of Centaurus.

HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24, it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of 105.4 light-years from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s. It has an absolute magnitude of 4.67.

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<span class="mw-page-title-main">HD 13189</span> Orange-hued star in the constellation Taurus

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HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.

<span class="mw-page-title-main">HD 10180</span> Star in the constellation Hydrus

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HD 100655 is a star in the zodiac constellation of Leo, located 449 light years away from the Sun. It has an apparent visual magnitude of +6.45, which makes it a challenge to see with the naked eye under ideal viewing conditions. The star is moving closer to the Earth with a heliocentric radial velocity of −5 km/s. It has one confirmed planet.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 Corben, P. M.; Stoy, R. H. (1968), "Photoelectric Magnitudes and Colours for Bright Southern Stars", Monthly Notes of the Astronomical Society of Southern Africa, 27: 11, Bibcode:1968MNSSA..27...11C.
  3. 1 2 3 4 5 6 7 8 Soubiran, C.; et al. (March 2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv: 0712.1370 , Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID   16602121.
  4. 1 2 3 4 5 6 7 8 9 10 Sato, Bun'ei; et al. (January 18, 2016), "A Pair of Giant Planets around the Evolved Intermediate-Mass Star HD 47366: Multiple Circular Orbits or a Mutually Retrograde Configuration", The Astrophysical Journal, 819 (1): 59, arXiv: 1601.04417 , Bibcode:2016ApJ...819...59S, doi: 10.3847/0004-637X/819/1/59 , S2CID   118535422.
  5. ↑ "HD 47366". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2016-01-21.
  6. ↑ Marshall, J. P.; et al. (January 2019), "Re-analyzing the Dynamical Stability of the HD 47366 Planetary System", The Astronomical Journal, 157 (1): 11, arXiv: 1811.06476 , Bibcode:2019AJ....157....1M, doi: 10.3847/1538-3881/aaef32 , S2CID   119449335, 1
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