HD 179070

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HD 179070
Observation data
Epoch J2000       Equinox J2000
Constellation Lyra [1]
Right ascension 19h 09m 26.8350s [2]
Declination +38° 42′ 50.456″ [2]
Apparent magnitude  (V)8.25 [3]
Characteristics
Evolutionary stage subgiant [4]
Spectral type F6 IV [4]
Apparent magnitude  (J)7.229±0.032 [5]
Apparent magnitude  (H)7.031±0.023 [5]
Apparent magnitude  (K)6.945±0.018 [5]
Variable type Planetary transit variable [4]
Astrometry
Radial velocity (Rv)−18.173599±0.00545 [6]  km/s
Proper motion (μ)RA: 28.093(18)  mas/yr [2]
Dec.: 28.546(20)  mas/yr [2]
Parallax (π)9.2181 ± 0.0173  mas [2]
Distance 353.8 ± 0.7  ly
(108.5 ± 0.2  pc)
Absolute magnitude  (MV)2.99 [7]
Details [8]
Mass 1.408+0.021
−0.030  M☉
Radius 1.902+0.018
−0.012  R☉
Luminosity 5.188+0.142
−0.128  L☉
Surface gravity (log g)4.026±0.004  cgs
Temperature 6,305±50  K
Metallicity [Fe/H]−0.03±0.10  dex
Rotation 12.62±0.03 d [3]
Rotational velocity (v sin i)8.4±0.5 [3]  km/s
Age 2.60±0.16  Gyr
Other designations
HIP  94112, Kepler-21, KOI-975, KIC  3632418, TYC  3120-963-1, 2MASS J19092683+3842505 [9]
Database references
SIMBAD data

HD 179070, also known as Kepler-21, is a star with a closely orbiting exoplanet in the northern constellation of Lyra. At an apparent visual magnitude of 8.25 this was the brightest star observed by the Kepler spacecraft to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018. [3] [10] This system is located at a distance of 354 light-years (109 parsecs ) from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s. [6]

The size of HD 179070 (right) compared to the Sun (left) Kepler-21.jpg
The size of HD 179070 (right) compared to the Sun (left)

The spectrum of HD 179070 presents as an evolving F-type subgiant star with a stellar classification of F6 IV. [4] This suggests the star has exhausted the supply of hydrogen at its core and is evolving into a giant star. It is an estimated 2.6 [8]  billion years old and is spinning with a rotation period of 12.6 days. [3] With 1.4 times the mass of the Sun it currently has 1.9 times the Sun's radius. The star is radiating five times the luminosity of the Sun from its photosphere at an effective temperature of 6,305 K. [8]

A faint nearby source was detected in 2011 and determined to be a co-moving stellar companion in 2016. Designated HD 179070 B, it lies at an angular separation of 0.75″ along a position angle of 129° relative to the primary. At the distance of this star, this corresponds to a projected separation of 87  AU . It is possible that this companion star had a significant influence on the exoplanet formation and subsequent orbital evolution. [11]

Planetary system

A candidate transiting exoplanet was discovered based from the first four months of photometry data from the Kepler spacecraft. [12] Confirmation was obtained in 2012 after extensive follow-up observations and analysis of the Kepler light curves. [4]

The calculated density of the planet is approximately 6.4 g·cm−3, similar to Earth's 5.5 g·cm−3, which suggests a rocky composition. With an equilibrium temperature of 2,025 Kelvin, the top few-hundred kilometers of the planet is probably molten. [3]

Calculations of the rate of orbital decay from tidal effects results in a decrease in the orbital period of 3.88 milliseconds per year, since this would be a change of only 4 seconds every thousand years it would be undetectable in any reasonable length of time. [13]

The HD 179070 planetary system [3] [14]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b7.5±1.3  M🜨 0.0427172±0.00000032.7858212±0.00000320.02±0.183.20+0.28
−0.26 ° 		1.639+0.019
−0.015  R🜨

Related Research Articles

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<span class="mw-page-title-main">HD 219134</span> Star in the constellation Cassiopeia

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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.

<span class="mw-page-title-main">HD 81040 b</span>

HD 81040 b is a massive gas giant exoplanet that orbits the star HD 81040, discovered in 2005 by radial velocity. Its orbital period is just over 1000 days. It has a semimajor axis of about 1.95 AU, and its orbit is quite eccentric, at a little over 0.5.

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 109749 is a binary star system about 206 light years away in the constellation of Centaurus. The pair have a combined apparent visual magnitude of 8.08, which is too faint to be visible to the naked eye. The primary component has a close orbiting exoplanet companion. The system is drifting closer with a heliocentric radial velocity of −13.2 km/s.

HD 179079 is a star with an exoplanetary companion in the equatorial constellation of Aquila. It has an apparent visual magnitude of approximately 7.96, making it too faint to be readily visible to the naked eye. The distance to this star can be determine using parallax measurements, which yields an estimate of approximately 228 light years. It is drifting further away with a radial velocity of +20 km/s.

Kepler-17 is a main-sequence yellow dwarf star that is much more active than the Sun with starspots covering roughly 6% of its surface. Starspots are long-lived, with at least one persisting for 1400 days.

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

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References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode: 1987PASP...99..695R . doi: 10.1086/132034 . Vizier query form
  2. 1 2 3 4 5 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 4 5 6 7 López-Morales, Mercedes; et al. (2016). "Kepler-21b: A Rocky Planet Around a V = 8.25 Magnitude Star". The Astronomical Journal. 152 (6). 204. arXiv: 1609.07617 . Bibcode: 2016AJ....152..204L . doi: 10.3847/0004-6256/152/6/204 .
  4. 1 2 3 4 5 Howell, Steve B.; et al. (2012). "Kepler-21b: A 1.6 REarth Planet Transiting the Bright Oscillating F Subgiant Star HD 179070". The Astrophysical Journal. 746 (2). 123. arXiv: 1112.2165 . Bibcode: 2012ApJ...746..123H . doi: 10.1088/0004-637X/746/2/123 .
  5. 1 2 3 Skrutskie, Michael F.; et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode: 2006AJ....131.1163S . doi: 10.1086/498708 . Vizier catalog entry
  6. 1 2 Jönsson, Henrik; et al. (August 17, 2020). "APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South". The Astronomical Journal. American Astronomical Society. 160 (3): 120. arXiv: 2007.05537 . Bibcode:2020AJ....160..120J. doi: 10.3847/1538-3881/aba592 . ISSN   1538-3881. S2CID   220496397.
  7. ↑ Holmberg, J.; et al. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics Supplement Series. 501 (3): 941–947. arXiv: 0811.3982 . Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. S2CID   118577511.
  8. 1 2 3 Silva Aguirre, V.; et al. (2015). "Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology". Monthly Notices of the Royal Astronomical Society. 452 (2): 2127–2148. arXiv: 1504.07992 . Bibcode: 2015MNRAS.452.2127S . doi: 10.1093/mnras/stv1388 .
  9. ↑ "HD 179070". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-06-10.
  10. ↑ Mayo, Andrew W.; et al. (2018). "275 Candidates and 149 Validated Planets Orbiting Bright Stars in K2 Campaigns 0–10". The Astronomical Journal. 155 (3). 136. arXiv: 1802.05277 . Bibcode: 2018AJ....155..136M . doi: 10.3847/1538-3881/aaadff .
  11. ↑ Ginski, C.; et al. (April 2012). "A lucky imaging multiplicity study of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 421 (3): 2498–2509. arXiv: 1202.4586 . Bibcode:2012MNRAS.421.2498G. doi:10.1111/j.1365-2966.2012.20485.x.
  12. ↑ Borucki, William J.; et al. (2011). "Characteristics of Planetary Candidates Observed by Kepler. II. Analysis of the First Four Months of Data". The Astrophysical Journal. 736 (1). 19. arXiv: 1102.0541 . Bibcode: 2011ApJ...736...19B . doi: 10.1088/0004-637X/736/1/19 .
  13. ↑ Luna, S. H.; et al. (September 2020). "The dynamical evolution of close-in binary systems formed by a super-Earth and its host star". Astronomy & Astrophysics. 641. A109. arXiv: 1907.10575 . Bibcode: 2020A&A...641A.109L . doi: 10.1051/0004-6361/201936551 .
  14. ↑ Bonomo, A. S.; Dumusque, X.; et al. (April 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems". Astronomy & Astrophysics . arXiv: 2304.05773 . doi:10.1051/0004-6361/202346211. S2CID   258078829.
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