| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Piscis Austrinus |
| Right ascension | 22h 55m 53.708s [1] |
| Declination | –26° 39′ 31.54″ [1] |
| Apparent magnitude (V) | 8.11 [2] |
| Characteristics | |
| Spectral type | K0V [2] or G9VCN+1 [3] |
| B−V color index | 0.821 [2] |
| Astrometry | |
| Radial velocity (Rv) | 31.141±0.0004 [4] km/s |
| Proper motion (μ) |
RA: 226.237
mas/
yr
[1] Dec.: −177.985 mas/ yr [1] |
| Parallax (π) | 27.2923 ± 0.0245 mas [1] |
| Distance | 119.5 ± 0.1
ly (36.64 ± 0.03 pc) |
| Absolute magnitude (MV) | 5.22 [2] |
| Details | |
| Mass | 0.74±0.07 [5] M☉ |
| Radius | 0.93±0.02 [5] R☉ |
| Luminosity | 0.79 [2] L☉ |
| Surface gravity (log g) | 4.37±0.04 [5] cgs |
| Temperature | 5,399±18 [5] K |
| Metallicity [Fe/H] | 0.27 [5] dex |
| Rotation | 35.6 d [2] |
| Rotational velocity (v sin i) | 1.4 [2] km/s |
| Age | 3.1 [2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 216770 is a star with an orbiting exoplanet in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 8.11, [2] 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. [4] The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.302 arcsec yr−1. [7]
The spectrum of HD 216770 presents as a late G-type main-sequence star, a yellow dwarf, with a stellar classification of G9VCN+1, [3] where the suffix notation indicates anomalously strong band of CN. The star is smaller than the Sun, with 74% of the Sun's mass and 93% of the Sun's radius. [5] It is about three billion years old and is spinning slowly with a rotation period of 35.6 days. [2] The abundance of iron, a measure of the metallicity of the star, is higher than solar. The star is radiating 79% of the luminosity of the Sun from its photosphere at an effective temperature of 5,399 K. [5]
In 2003 an exoplanet was announced orbiting it by the Geneva Extrasolar Planet Search team. [2] As the inclination of the orbital plane is unknown, only a lower bound on the mass of the object can be determined. It has at least 65% of the mass of Jupiter. The body has an eccentric orbit with a period of 118.5 days.
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >0.65 MJ | 0.46 | 118.45 ± 0.55 | 0.37 ± 0.06 | — | — |
- ^ a b c d 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.
- ^ a b c d e f g h i j k Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv: astro-ph/0310316. Bibcode: 2004A&A...415..391M. doi: 10.1051/0004-6361:20034250. S2CID 5233877.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv: astro-ph/0603770. Bibcode: 2006AJ....132..161G. doi: 10.1086/504637. S2CID 119476992.
- ^ a b 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.
- ^ a b c d e f g Stassun, Keivan G.; et al. (2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv: 1609.04389. Bibcode: 2017AJ....153..136S. doi: 10.3847/1538-3881/aa5df3. S2CID 119219062.
- ^ "HD 216770". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-06-25.
- ^ Luyten, W. J. (June 1995). "NLTT Catalogue (Luyten, 1979)". VizieR Online Data Catalog. Bibcode: 1995yCat.1098....0L.
- "Notes for star HD 216770". Extrasolar Planets Encyclopaedia. Archived from the original on June 2, 2006.
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| Galaxies |
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Piscis Austrinus |
| Right ascension | 22h 55m 53.708s [1] |
| Declination | –26° 39′ 31.54″ [1] |
| Apparent magnitude (V) | 8.11 [2] |
| Characteristics | |
| Spectral type | K0V [2] or G9VCN+1 [3] |
| B−V color index | 0.821 [2] |
| Astrometry | |
| Radial velocity (Rv) | 31.141±0.0004 [4] km/s |
| Proper motion (μ) |
RA: 226.237
mas/
yr
[1] Dec.: −177.985 mas/ yr [1] |
| Parallax (π) | 27.2923 ± 0.0245 mas [1] |
| Distance | 119.5 ± 0.1
ly (36.64 ± 0.03 pc) |
| Absolute magnitude (MV) | 5.22 [2] |
| Details | |
| Mass | 0.74±0.07 [5] M☉ |
| Radius | 0.93±0.02 [5] R☉ |
| Luminosity | 0.79 [2] L☉ |
| Surface gravity (log g) | 4.37±0.04 [5] cgs |
| Temperature | 5,399±18 [5] K |
| Metallicity [Fe/H] | 0.27 [5] dex |
| Rotation | 35.6 d [2] |
| Rotational velocity (v sin i) | 1.4 [2] km/s |
| Age | 3.1 [2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 216770 is a star with an orbiting exoplanet in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 8.11, [2] 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. [4] The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.302 arcsec yr−1. [7]
The spectrum of HD 216770 presents as a late G-type main-sequence star, a yellow dwarf, with a stellar classification of G9VCN+1, [3] where the suffix notation indicates anomalously strong band of CN. The star is smaller than the Sun, with 74% of the Sun's mass and 93% of the Sun's radius. [5] It is about three billion years old and is spinning slowly with a rotation period of 35.6 days. [2] The abundance of iron, a measure of the metallicity of the star, is higher than solar. The star is radiating 79% of the luminosity of the Sun from its photosphere at an effective temperature of 5,399 K. [5]
In 2003 an exoplanet was announced orbiting it by the Geneva Extrasolar Planet Search team. [2] As the inclination of the orbital plane is unknown, only a lower bound on the mass of the object can be determined. It has at least 65% of the mass of Jupiter. The body has an eccentric orbit with a period of 118.5 days.
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >0.65 MJ | 0.46 | 118.45 ± 0.55 | 0.37 ± 0.06 | — | — |
- ^ a b c d 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.
- ^ a b c d e f g h i j k Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv: astro-ph/0310316. Bibcode: 2004A&A...415..391M. doi: 10.1051/0004-6361:20034250. S2CID 5233877.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv: astro-ph/0603770. Bibcode: 2006AJ....132..161G. doi: 10.1086/504637. S2CID 119476992.
- ^ a b 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.
- ^ a b c d e f g Stassun, Keivan G.; et al. (2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv: 1609.04389. Bibcode: 2017AJ....153..136S. doi: 10.3847/1538-3881/aa5df3. S2CID 119219062.
- ^ "HD 216770". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-06-25.
- ^ Luyten, W. J. (June 1995). "NLTT Catalogue (Luyten, 1979)". VizieR Online Data Catalog. Bibcode: 1995yCat.1098....0L.
- "Notes for star HD 216770". Extrasolar Planets Encyclopaedia. Archived from the original on June 2, 2006.
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| Galaxies |
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