HD 220773

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HD 220773
Observation data
Epoch J2000       Equinox J2000
Constellation Pegasus [1]
Right ascension 23h 26m 27.445s [2]
Declination +08° 38′ 37.84″ [2]
Apparent magnitude  (V)7.10 [1]
Characteristics
Evolutionary stage main sequence
Spectral type G0 V [3] or F9 V [4]
B−V color index 0.602±0.005 [1]
Astrometry
Radial velocity (Rv)−37.735±0.0009 [5]  km/s
Proper motion (μ)RA: 27.096  mas/yr [2]
Dec.: −222.458  mas/yr [2]
Parallax (π)19.7694 ± 0.0669  mas [2]
Distance 165.0 ± 0.6  ly
(50.6 ± 0.2  pc)
Absolute magnitude  (MV)3.57 [1]
Details
Mass 1.154±0.003 [6]   M☉
Radius 1.73±0.02 [6]   R☉
Luminosity 3.16±0.01 [6]   L☉
Surface gravity (log g)4.02±0.01 [6]   cgs
Temperature 5,852±26 [6]   K
Metallicity [Fe/H]0.09±0.06 [7]   dex
Rotational velocity (v sin i)3.82±1.00 [8]  km/s
Age 6.3±0.1 [6]   Gyr
Other designations
BD+07 5030, Gaia DR2  2761142326076104192, HD  220773, HIP  115697, SAO  128181, 2MASS J23262744+0838376 [9]
Database references
SIMBAD data

HD 220773 is a star in the northern constellation of Pegasus. It has an apparent visual magnitude of 7.10, [1] which is too faint to be visible with the naked eye. The distance to this system, as determined by parallax measurements, is 165  light years, [2] but it is drifting closer with a radial velocity of −37.7 km/s. [5] The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.187 arcsec yr−1. [10]

The spectrum of HD 220773 presents as a late type star F-type or early G-type main-sequence star with a stellar classification of F9 V [4] or G0 V, [3] respectively. It is older than the Sun, with an estimated age of 6.3 billion years, [6] and the magnetic activity in the chromosphere is at a low level. [7] The star has 15% greater mass than the Sun but the radius is 73% larger. [6] The abundance of iron, a measure of the star's metallicity, is slightly higher than solar. [7] It is radiating over three times the luminosity of the Sun from its photosphere at an effective temperature of 5,852 K. [6]

A survey in 2015 ruled out the existence of any additional stellar companions at projected distances from 31 to 337 astronomical units. [3]

Search for planets

The detection of an exoplanet, HD 220773 b, by the radial velocity method was claimed in 2012 based on observations at the McDonald Observatory. As the inclination of the orbital plane is unknown, only a lower bound on the mass can be determined. This object has at least 1.45 times the mass of Jupiter. It has a very eccentric orbit with a semimajor axis of around 5  AU , taking 10.2 years to complete an orbit. [7]

However, a follow-up study in 2024 found no evidence of this planet in radial velocity data from the HARPS-N spectrograph. In addition, astrometric data from the Gaia space telescope also shows no evidence of a companion, placing an upper limit on the mass of any planet at 5 AU consistent with the claimed minimum mass of planet b. The McDonald team stated that their data collected since 2012 is also no longer consistent with the claimed planet. [11]

Related Research Articles

HD 216770 is a star with an orbiting exoplanet in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 8.11, it is too faint to be visible to the naked eye. It is located at a distance of 120 light years from the Sun, as determined by parallax measurements, and is drifting further away with a radial velocity of 31.1 km/s. The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.302 arcsec yr−1.

HD 114783 is a star with two exoplanetary companions in the equatorial constellation of Virgo. With an apparent visual magnitude of 7.56 it is too faint to be visible with the unaided eye, but is an easy target for binoculars. Based on parallax measurements, it is located at a distance of 68.6 light-years from the Sun, but is drifting closer with a radial velocity of −12 km/s.

HD 114386 is a star with a pair of orbiting exoplanets in the southern constellation of Centaurus. It has an apparent visual magnitude of 8.73, which means it cannot be viewed with the naked eye but can be seen with a telescope or good binoculars. Based on parallax measurements, the system is located at a distance of 91 light years from the Sun. It is receding with a radial velocity of 33.4 km/s. The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.318 arcsec yr−1.

HD 130322 is a star with a close orbiting exoplanet in the constellation of Virgo. The distance to this system is 104 light years, as determined using parallax measurements. It is drifting closer to the Sun with a radial velocity of −12.4 km/s. With an apparent visual magnitude of 8.04, it is too dim to be visible to the naked eye; requiring binoculars or a small telescope to view. Being almost exactly on the celestial equator the star is visible everywhere in the world except for the North Pole. The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.197 arcsec yr−1.

HD 142 is a wide binary star system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7. The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.

HD 81040 is a star in the equatorial constellation of Leo. With an apparent visual magnitude of +7.73 it is too dim to be visible to the naked eye but can be viewed with a small telescope. The star is located at a distance of 112 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +49 km/s, having come to within 48 light-years some 527,000 years ago.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

HD 210702 is a star with an orbiting exoplanet in the northern constellation of Pegasus. It has an apparent visual magnitude of 5.93, which is bright enough that the star is dimly visible to the naked eye. The distance to HD 210702 is 177 light years based on parallax measurements, and it is drifting further away with a radial velocity of 18.5 km/s. It is a probable member of the Ursa Major moving group, an association of co-moving stars.

HD 43691 is a star with an orbiting exoplanet in the constellation Auriga. With an apparent visual magnitude of 8.03, it is too faint to be visible to the naked eye. This system is located at a distance of 279 light years based on parallax measurements, but is drifting closer with a heliocentric radial velocity of −29 km/s.

HD 106252 is a star with a brown dwarf companion in the constellation Virgo. An apparent visual magnitude of 7.41 means this star is too faint to be visible to the naked eye. It is located at a distance of 210 light years from the Sun based on parallax measurements, and is receding with a radial velocity of 15 km/s.

HD 149143, also called Rosalíadecastro, is a star with a close orbiting exoplanet in the Ophiuchus constellation. Its apparent visual magnitude is 7.89 and the absolute magnitude is 3.87. The system is located at a distance of 239 light years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 12 km/s.

HD 212301 is a binary star system in the south circumpolar constellation of Octans. This star is also called HIP 110852. With an apparent visual magnitude of 7.76, it is too faint to be visible to the naked eye. The system is located at a distance of 177 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.7 km/s. It has an absolute magnitude of 4.06.

HD 47186 is a star with a pair of orbiting exoplanets in the southern constellation of Canis Major. The system is located at a distance of 122 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of 4.2 km/s. Although it has an absolute magnitude of 4.64, at the distance of this system the apparent visual magnitude is 7.63; too faint to be seen with the naked eye. It has a high proper motion, traversing the celestial sphere at an angular rate of 0.272″·yr−1.

HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

HD 164604 is a single star in the southern constellation of Sagittarius constellation. It has the proper name Pincoya, as selected in the NameExoWorlds campaign by Chile, during the 100th anniversary of the IAU. Pincoya is a female water spirit from southern Chilean mythology who is said to bring drowned sailors to the Caleuche so that they can live in the afterlife. A 2015 survey ruled out the existence of any additional stellar companions at projected distances from 13 to 340 astronomical units. It is known to host a single super-Jupiter exoplanet.

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.

HD 79498 is a double star in the northern constellation of Cancer. The primary component of this pair has an orbiting exoplanet companion. This star is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.05. The system is located at a distance of 159 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 20 km/s. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.2″·yr−1.

HD 98649 is a star with an orbiting exoplanet in the southern Crater constellation. Based on parallax measurements, it is located at a distance of 137.5 light years from the Sun. The system is drifting further away with a heliocentric radial velocity of 4.3 km/s. With an apparent visual magnitude of +8.00, it is too faint to be viewed with the naked eye. The system has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.24″·yr−1.

HD 106515 is a binary star in the constellation of Virgo.

HD 197037 is a binary star system. Its primary or visible star, HD 197037 A, is a F-type main-sequence star. Its surface temperature is 6150±34 K. HD 197037 A is depleted in heavy elements compared to the Sun, with a metallicity Fe/H index of −0.16±0.03, but is younger at an age of 3.408±0.924 billion years.

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 Mugrauer, M.; Ginski, C. (12 May 2015). "High-contrast imaging search for stellar and substellar companions of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 450 (3): 3127–3136. Bibcode:2015MNRAS.450.3127M. doi: 10.1093/mnras/stv771 . hdl: 1887/49340 .
  4. 1 2 Wittrock, Justin M.; et al. (2017). "Exclusion of Stellar Companions to Exoplanet Host Stars". The Astronomical Journal. 154 (5): 184. arXiv: 1709.05315 . Bibcode:2017AJ....154..184W. doi: 10.3847/1538-3881/aa8d69 . S2CID   55789971.
  5. 1 2 Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv: 1804.09370 . Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID   52952408.
  6. 1 2 3 4 5 6 7 8 9 Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv: 1511.01744 . Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID   53971692. A5.
  7. 1 2 3 4 Robertson, Paul; et al. (2012). "The McDonald Observatory Planet Search: New Long-period Giant Planets and Two Interacting Jupiters in the HD 155358 System". The Astrophysical Journal. 749 (1): 39. arXiv: 1202.0265 . Bibcode:2012ApJ...749...39R. doi:10.1088/0004-637X/749/1/39. S2CID   59273311.
  8. ↑ Tejada Arevalo, Roberto A.; et al. (October 2021). "Further Evidence for Tidal Spin-up of Hot Jupiter Host Stars". The Astrophysical Journal. 919 (2): 138. arXiv: 2107.05759 . Bibcode:2021ApJ...919..138T. doi: 10.3847/1538-4357/ac1429 . 138.
  9. ↑ "HD 220773". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 18 September 2020.
  10. ↑ Luyten, W. J. (June 1995). "NLTT Catalogue (Luyten, 1979)". VizieR Online Data Catalog. Bibcode:1995yCat.1098....0L.
  11. ↑ Carleo, Ilaria; Desidera, Silvano; et al. (June 2024). "Disproving the High-eccentricity Planet HD 220773b". Research Notes of the AAS . 8 (6): 161. doi: 10.3847/2515-5172/ad57b5 .
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