| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 06h 12m 00.567s [1] |
| Declination | +06° 46′ 59.06″ [1] |
| Apparent magnitude (V) | 6.85 [2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | G4V [3] |
| B−V color index | 0.642±0.007 [2] |
| Astrometry | |
| Radial velocity (Rv) | −53.52±0.14 [4] km/s |
| Proper motion (μ) |
RA: 197.247
mas/
yr
[1] Dec.: −254.867 mas/ yr [1] |
| Parallax (π) | 40.9764 ± 0.0240 mas [1] |
| Distance | 79.60 ± 0.05
ly (24.40 ± 0.01 pc) |
| Absolute magnitude (MV) | 5.03±0.06 [3] |
| Details | |
| Mass | 0.92±0.02 [5] M☉ |
| Radius | 0.94 [5] R☉ |
| Luminosity | 0.918±0.012 [5] L☉ |
| Surface gravity (log g) | 4.44±0.01 [6] cgs |
| Temperature | 5,758±5 K
[6] 5,765±17 [5] K |
| Metallicity [Fe/H] | −0.096±0.005 dex
[6] −0.10±0.02 [5] dex |
| Rotation | 16.9 d [7] |
| Rotational velocity (v sin i) | 1.83±0.11 [6] km/s |
| Age | 5.51±0.71 Gyr
[6] 5.5±0.2 [5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 42618 is a well-studied [7] star with an exoplanetary companion in the equatorial constellation of Orion. With an apparent visual magnitude of 6.85 [2] it is too faint to be readily visible to the naked eye. This system is located at a distance of 79.6 light years from the Sun based on parallax measurements. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.321 ″ per year. [9] HD 42618 is drifting closer with a radial velocity of −53.5 [4] km/s and is predicted to come as near as 42.6 light-years in around 297,000 years. [2]
The stellar classification of HD 42618 is G4V, [3] which shows it to be an ordinary G-type main-sequence star. It is considered a close solar analog, which means the physical properties of the star are particularly similar to those of the Sun. [10] Seismic model indicates the star is older and more evolved than the Sun with an age of about 5.5 billion years. [5] It is spinning with a low projected rotational velocity of 1.8 km/s, [6] with the rotation rate being consistent with the star's low activity level. [11] The star has 92% of the mass of the Sun and 94% of the Sun's radius. The surface metallicity is lower than in the Sun, [5] with the abundance patterns being consistent with a solar-type star. [11] HD 42618 is radiating 92% of the luminosity of the Sun from its photosphere at an effective temperature of 5,765 K. [5]
In 2016, the discovery of a candidate exoplanet companion orbiting HD 42618 was announced. Designated HD 42618 b, it was found using the radial velocity method which showed a periodicity of 149.6 days. The orbital elements have the planet orbiting at a distance of 0.55 AU from the host star with an orbital eccentricity (ovalness) of 0.2 and a Neptune-like mass. A second signal with a period of 388 days was detected, but this is unconfirmed and may be false. A 4,850 day signal is likely the result of star's magnetic activity cycle. [7]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 14.4+2.5 −2.4 M🜨 |
0.554±0.011 | 149.61+0.37 −0.34 |
0.19+0.15 −0.12 |
— | — |
- ^ a b c d 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.
- ^ 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.
- ^ a b c Medhi, B. J.; et al. (July 2007), "Results from a spectroscopic survey in the CoRoT fields. I. Search for chromospherically active stars", Astronomy and Astrophysics, 469 (2): 713–719, Bibcode: 2007A&A...469..713M, doi: 10.1051/0004-6361:20054173.
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f g h i Castro, M.; et al. (August 2021), "Modeling of two CoRoT solar analogues constrained by seismic and spectroscopic analysis", Monthly Notices of the Royal Astronomical Society, 505 (2): 2151–2158, arXiv: 2008.01163, Bibcode: 2021MNRAS.505.2151C, doi: 10.1093/mnras/stab1410.
- ^ a b c d e f dos Santos, Leonardo A.; et al. (August 2016), "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars", Astronomy & Astrophysics, 592: 8, arXiv: 1606.06214, Bibcode: 2016A&A...592A.156D, doi: 10.1051/0004-6361/201628558, S2CID 53533614, A156.
- ^ a b c d Fulton, Benjamin J.; et al. (October 2016), "Three Temperate Neptunes Orbiting Nearby Stars", The Astrophysical Journal, 830 (1): 19, arXiv: 1607.00007, Bibcode: 2016ApJ...830...46F, doi: 10.3847/0004-637X/830/1/46, S2CID 36666883, 46.
- ^ "HD 42618", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2022-02-17.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv: astro-ph/0412070, Bibcode: 2005AJ....129.1483L, doi: 10.1086/427854, S2CID 2603568.
- ^ Soubiran, C.; Triaud, A. (May 2004), "The Top Ten solar analogs in the ELODIE library", Astronomy and Astrophysics, 418 (3): 1089–1100, arXiv: astro-ph/0402094, Bibcode: 2004A&A...418.1089S, doi: 10.1051/0004-6361:20035708.
- ^ a b Morel, T.; et al. (April 2013), "Abundance study of the two solar-analogue CoRoT targets HD 42618 and HD 43587 from HARPS spectroscopy", Astronomy & Astrophysics, 552: 10, arXiv: 1302.3172, Bibcode: 2013A&A...552A..42M, doi: 10.1051/0004-6361/201220883, S2CID 53686102, A42.
- Castro, M.; Baudin, F.; Marques, J.; do Nascimento Jr., J. D. (2018), "The impact of GAIA astrometry on the evolutionary status of the seismic analog HD 42618" (PDF), Boletim da Sociedade Astronômica Brasileira, 30 (1): 93–94, retrieved 2022-02-17.
- Barban, C.; et al. (June 2013), "Solar-like oscillations in distant stars as seen by CoRoT : the special case of HD 42618, a solar sister", Journal of Physics: Conference Series, 440 (1): 012030, Bibcode: 2013JPhCS.440a2030B, doi: 10.1088/1742-6596/440/1/012030, 012030.
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 06h 12m 00.567s [1] |
| Declination | +06° 46′ 59.06″ [1] |
| Apparent magnitude (V) | 6.85 [2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | G4V [3] |
| B−V color index | 0.642±0.007 [2] |
| Astrometry | |
| Radial velocity (Rv) | −53.52±0.14 [4] km/s |
| Proper motion (μ) |
RA: 197.247
mas/
yr
[1] Dec.: −254.867 mas/ yr [1] |
| Parallax (π) | 40.9764 ± 0.0240 mas [1] |
| Distance | 79.60 ± 0.05
ly (24.40 ± 0.01 pc) |
| Absolute magnitude (MV) | 5.03±0.06 [3] |
| Details | |
| Mass | 0.92±0.02 [5] M☉ |
| Radius | 0.94 [5] R☉ |
| Luminosity | 0.918±0.012 [5] L☉ |
| Surface gravity (log g) | 4.44±0.01 [6] cgs |
| Temperature | 5,758±5 K
[6] 5,765±17 [5] K |
| Metallicity [Fe/H] | −0.096±0.005 dex
[6] −0.10±0.02 [5] dex |
| Rotation | 16.9 d [7] |
| Rotational velocity (v sin i) | 1.83±0.11 [6] km/s |
| Age | 5.51±0.71 Gyr
[6] 5.5±0.2 [5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 42618 is a well-studied [7] star with an exoplanetary companion in the equatorial constellation of Orion. With an apparent visual magnitude of 6.85 [2] it is too faint to be readily visible to the naked eye. This system is located at a distance of 79.6 light years from the Sun based on parallax measurements. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.321 ″ per year. [9] HD 42618 is drifting closer with a radial velocity of −53.5 [4] km/s and is predicted to come as near as 42.6 light-years in around 297,000 years. [2]
The stellar classification of HD 42618 is G4V, [3] which shows it to be an ordinary G-type main-sequence star. It is considered a close solar analog, which means the physical properties of the star are particularly similar to those of the Sun. [10] Seismic model indicates the star is older and more evolved than the Sun with an age of about 5.5 billion years. [5] It is spinning with a low projected rotational velocity of 1.8 km/s, [6] with the rotation rate being consistent with the star's low activity level. [11] The star has 92% of the mass of the Sun and 94% of the Sun's radius. The surface metallicity is lower than in the Sun, [5] with the abundance patterns being consistent with a solar-type star. [11] HD 42618 is radiating 92% of the luminosity of the Sun from its photosphere at an effective temperature of 5,765 K. [5]
In 2016, the discovery of a candidate exoplanet companion orbiting HD 42618 was announced. Designated HD 42618 b, it was found using the radial velocity method which showed a periodicity of 149.6 days. The orbital elements have the planet orbiting at a distance of 0.55 AU from the host star with an orbital eccentricity (ovalness) of 0.2 and a Neptune-like mass. A second signal with a period of 388 days was detected, but this is unconfirmed and may be false. A 4,850 day signal is likely the result of star's magnetic activity cycle. [7]
| Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 14.4+2.5 −2.4 M🜨 |
0.554±0.011 | 149.61+0.37 −0.34 |
0.19+0.15 −0.12 |
— | — |
- ^ a b c d 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.
- ^ 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.
- ^ a b c Medhi, B. J.; et al. (July 2007), "Results from a spectroscopic survey in the CoRoT fields. I. Search for chromospherically active stars", Astronomy and Astrophysics, 469 (2): 713–719, Bibcode: 2007A&A...469..713M, doi: 10.1051/0004-6361:20054173.
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f g h i Castro, M.; et al. (August 2021), "Modeling of two CoRoT solar analogues constrained by seismic and spectroscopic analysis", Monthly Notices of the Royal Astronomical Society, 505 (2): 2151–2158, arXiv: 2008.01163, Bibcode: 2021MNRAS.505.2151C, doi: 10.1093/mnras/stab1410.
- ^ a b c d e f dos Santos, Leonardo A.; et al. (August 2016), "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars", Astronomy & Astrophysics, 592: 8, arXiv: 1606.06214, Bibcode: 2016A&A...592A.156D, doi: 10.1051/0004-6361/201628558, S2CID 53533614, A156.
- ^ a b c d Fulton, Benjamin J.; et al. (October 2016), "Three Temperate Neptunes Orbiting Nearby Stars", The Astrophysical Journal, 830 (1): 19, arXiv: 1607.00007, Bibcode: 2016ApJ...830...46F, doi: 10.3847/0004-637X/830/1/46, S2CID 36666883, 46.
- ^ "HD 42618", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2022-02-17.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv: astro-ph/0412070, Bibcode: 2005AJ....129.1483L, doi: 10.1086/427854, S2CID 2603568.
- ^ Soubiran, C.; Triaud, A. (May 2004), "The Top Ten solar analogs in the ELODIE library", Astronomy and Astrophysics, 418 (3): 1089–1100, arXiv: astro-ph/0402094, Bibcode: 2004A&A...418.1089S, doi: 10.1051/0004-6361:20035708.
- ^ a b Morel, T.; et al. (April 2013), "Abundance study of the two solar-analogue CoRoT targets HD 42618 and HD 43587 from HARPS spectroscopy", Astronomy & Astrophysics, 552: 10, arXiv: 1302.3172, Bibcode: 2013A&A...552A..42M, doi: 10.1051/0004-6361/201220883, S2CID 53686102, A42.
- Castro, M.; Baudin, F.; Marques, J.; do Nascimento Jr., J. D. (2018), "The impact of GAIA astrometry on the evolutionary status of the seismic analog HD 42618" (PDF), Boletim da Sociedade Astronômica Brasileira, 30 (1): 93–94, retrieved 2022-02-17.
- Barban, C.; et al. (June 2013), "Solar-like oscillations in distant stars as seen by CoRoT : the special case of HD 42618, a solar sister", Journal of Physics: Conference Series, 440 (1): 012030, Bibcode: 2013JPhCS.440a2030B, doi: 10.1088/1742-6596/440/1/012030, 012030.
| Stars |
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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
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Star clusters |
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| Nebulae |
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| Galaxies |
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