Kepler-432

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Kepler-432
Observation data
Epoch J2000       Equinox J2000
Constellation Cygnus
Right ascension 19h 33m 07.7292s [1]
Declination +48° 17′ 09.1454″ [1]
Apparent magnitude  (V)13
Characteristics
Evolutionary stage Giant star + Main sequence
Spectral type K2III [2] + M?V [3]
Astrometry
Proper motion (μ)RA: 4.667(12)  mas/yr [1]
Dec.: 9.963(11)  mas/yr [1]
Parallax (π)1.1712 ± 0.0097  mas [1]
Distance 2,780 ± 20  ly
(854 ± 7  pc)
Orbit
PrimaryKepler-432 A
CompanionKepler-432 B
Period (P)15,000 yr
Details [3]
Kepler-432 A
Mass 1.32+0.10
−0.07  M☉
Radius 4.06+0.12
−0.08  R☉
Luminosity 9.206 ± 0.01  L☉
Surface gravity (log g)3.345 ± 0.006  cgs
Temperature 4995 ± 78  K
Metallicity [Fe/H]0.176 ± 0.07  dex
Rotational velocity (v sin i)2.7 ± 0.5 km/s
Age 4.2+0.8
−1.0  Gyr
Kepler-432 B
Mass ~0.52  M☉
Temperature ~3660  K
Age 4.2?  Gyr
Position (relative to Kepler-432 A) [3]
ComponentKepler-432 B
Projected separation ~750 AU [3]
Other designations
Gaia DR2  2128901871432519936, KOI-1299, KIC  10864656, 2MASS J19330772+4817092 [4]
Database references
SIMBAD data
KIC data

Kepler-432 is a binary star system with at least two planets in orbit around the primary companion, located about 2,780 light-years away from Earth.

Contents

Nomenclature and history

The Kepler Space Telescope search volume, in the context of the Milky Way Galaxy. LombergA1024.jpg
The Kepler Space Telescope search volume, in the context of the Milky Way Galaxy.

Prior to Kepler observation, Kepler-432 had the 2MASS catalogue number 2MASS J19330772+4817092. In the Kepler Input Catalog it has the designation of KIC 10864656, and when it was found to have transiting planet candidates it was given the Kepler object of interest number of KOI-1299.

Planetary candidates were detected around the star by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars. These dips in brightness can be interpreted as planets whose orbits pass in front of their stars from the perspective of Earth, although other phenomenon can also be responsible which is why the term planetary candidate is used. [5]

Following the acceptance of the discovery paper, the Kepler team provided an additional moniker for the system of "Kepler-432". [6] The discoverers referred to the star as Kepler-432, which is the normal procedure for naming the exoplanets discovered by the spacecraft. [2] Hence, this is the name used by the public to refer to the star and its planet.

Candidate planets that are associated with stars studied by the Kepler Mission are assigned the designations ".01", ".02" etc. after the star's name, in the order of discovery. [7] If planet candidates are detected simultaneously, then the ordering follows the order of orbital periods from shortest to longest. [7] Following these rules, there was two candidate planets detected, with orbital periods of 52.501129 and 406.2 days.

The designation b and c derive from the order of discovery. The designation of b is given to the first planet orbiting a given star, and c to the farthest. [8] In the case of Kepler-432, there was initially two detected, so the letters b and c are used. The planets are more commonly referred to without the "A" designation, although sometimes the full designation is used.

Stellar characteristics

Kepler-432 is a binary star system composed of a K-type giant star (Kepler-432 A) and a red dwarf star (Kepler-432 B).

The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.

Kepler-432 A

Kepler-432 A is a K-type giant star. It has exhausted the hydrogen in its core and has begun expanding into a red giant. [3] The star has a mass and radius 132% and 406% that of the Sun. It has a temperature of 4995 K and is 4.2 billion years old. In comparison, the Sun is about 4.6 billion years old [9] and has a temperature of 5778 K. [10]

The primary star is metal-rich, with a metallicity ([Fe/H]) of about 0.17, or about 147% of the amount of iron and other heavier metals found in the Sun. [3] Its luminosity is typical for an evolving giant star like Kepler-432, with a luminosity about 9.3 times the solar luminosity. [3]

The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.

Kepler-432 B

Kepler-432 B is a red dwarf companion with an estimated mass 36% that of the Sun and an estimated temperature of 3660 K. The projected separation is estimated to be around 750 AU. [3]

Planetary system

The Kepler-432 A planetary system [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 5.41+0.32
−0.8  MJ 		0.301 ± 0.01452.5011290.5134 ± 0.0188.17+0.61
−0.33 ° 		1.45 ± 0.039  RJ
c 2.43+0.22
−0.24  MJ 		1.1?406.2+3.9
−2.5		———

The primary companion is known to host 2 giant planets, both more massive than Jupiter. The innermost planet, Kepler-432b, is interacting with its star and is slowly spiraling inwards towards its star as a result of tidal interaction. [2] It will probably be devoured by its star as it expands past the orbit of planet b. The outermost planet was only detected through radial velocity and hence only its mass is known. [3]

Related Research Articles

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<span class="mw-page-title-main">Kepler-35</span> Binary star system in the constellation Cygnus

Kepler-35 is a binary star system in the constellation of Cygnus. These stars, called Kepler-35A and Kepler-35B have masses of 89% and 81% solar masses respectively, and both are assumed to be of spectral class G. They are separated by 0.176 AU, and complete an eccentric orbit around a common center of mass every 20.73 days.

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<span class="mw-page-title-main">PH2</span> Star in the constellation Cygnus

PH2, also known as Kepler-86, or KIC 12735740, is a G-type star 1,120 light-years distant within the constellation Cygnus. Roughly the size and temperature of the Sun, PH2 gained prominence when it was known to be the host of one of 42 planet candidates detected by the Planet Hunters citizen science project in its second data release. The candidate orbiting around PH2, known as PH2b, had been determined to have a spurious detection probability of only 0.08%, thus effectively confirming its existence as a planet.

<span class="mw-page-title-main">Kepler-62</span> K-type star in the constellation Lyra

Kepler-62 is a K-type main sequence star cooler and smaller than the Sun, located roughly 980 light-years from Earth in the constellation Lyra. It resides within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. On April 18, 2013, it was announced that the star has five planets, two of which, Kepler-62e and Kepler-62f are within the star's habitable zone. The outermost, Kepler-62f, is likely a rocky planet.

<span class="mw-page-title-main">Kepler-69</span> Star in the constellation Cygnus

Kepler-69 is a G-type main-sequence star similar to the Sun in the constellation Cygnus, located about 2,430 ly (750 pc) from Earth. On April 18, 2013 it was announced that the star has two planets. Although initial estimates indicated that the terrestrial planet Kepler-69c might be within the star's habitable zone, further analysis showed that the planet very likely is interior to the habitable zone and is far more analogous to Venus than to Earth and thus completely inhospitable.

<span class="mw-page-title-main">Kepler-90</span> Star in the constellation Draco, orbited by eight planets

Kepler-90, also designated 2MASS J18574403+4918185, is a F-type star located about 2,790 light-years (855 pc) from Earth in the constellation of Draco. It is notable for possessing a planetary system that has the same number of observed planets as the Solar System.

Kepler-61 is a K-type main-sequence star approximately 1,100 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. On April 24, 2013 it was announced that the star has an extrasolar planet orbiting in the inner edge of the habitable zone, named Kepler-61b.

<span class="mw-page-title-main">Kepler-138</span> Red dwarf in the constellation Lyra

Kepler-138, also known as KOI-314, is a red dwarf located in the constellation Lyra, 219 light years from Earth. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets transiting their stars.

Kepler-432b (also known by its Kepler Object of Interest designation KOI-1299.01) is a hot super-Jupiter (or "warm" super-Jupiter) exoplanet orbiting the giant star Kepler-432 A, the innermost of two such planets discovered by NASA's Kepler spacecraft. It is located about 2,830 light-years (870 parsecs, or nearly 2.684×1016 km) from Earth in the constellation Cygnus. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured.

<span class="mw-page-title-main">Kepler-452</span> G-type main-sequence star in the constellation Cygnus

Kepler-452 is a G-type main-sequence star located about 1,810 light-years away from Earth in the Cygnus constellation. Although similar in temperature to the Sun, it is 20% brighter, 3.7% more massive and 11% larger. Alongside this, the star is approximately six billion years old and possesses a high metallicity.

Kepler-1229 is a red dwarf star located about 870 light-years (270 pc) away from the Earth in the constellation of Cygnus. It is known to host a super-Earth exoplanet within its habitable zone, Kepler-1229b, which was discovered in 2016.

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Kepler-419 is an F-type main-sequence star located about 3,400 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. In 2012, a potential planetary companion in a very eccentric orbit was detected around this star, but its planetary nature was not confirmed until 12 June 2014, when it was named Kepler-419b. A second planet was announced orbiting further out from the star in the same paper, named Kepler-419c.

<span class="mw-page-title-main">K2-33</span> Star in the constellation Scorpius

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<span class="mw-page-title-main">HD 179070</span> Star in the constellation Lyra

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. This system is located at a distance of 354 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s.

Kepler-1708b is a Jupiter-sized exoplanet orbiting the Sun-like star Kepler-1708, located in the constellation of Cygnus approximately 5,600 light years away from Earth. It was first detected in 2011 by NASA's Kepler mission using the transit method, but was not identified as a candidate planet until 2019. In 2021, a candidate Neptune-sized exomoon in orbit around Kepler-1708b was found by astronomer David Kipping and colleagues in an analysis using Kepler transit data. However, subsequent research has raised discrepancies about the possible existence of an exomoon, similar to that of Kepler-1625b.

References

  1. 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.
  2. 1 2 3 Ortiz, Mauricio; Gandolfi, Davide; Reffert, Sabine; Quirrenbach, Andreas; Deeg, Hans J.; Karjalainen, Raine; Montañes-Rodríguez, Pilar; Nespral, David; Nowak, Grzegorz; Osorio, Yeisson; Palle, Enric (2015). "Kepler-432 b: A massive warm Jupiter in a 52-day eccentric orbit transiting a giant star". Astronomy & Astrophysics. 573 (6): L6. arXiv: 1410.3000 . Bibcode:2015A&A...573L...6O. doi:10.1051/0004-6361/201425146. S2CID   11379442.
  3. 1 2 3 4 5 6 7 8 9 10 Quinn, Samuel N.; White, Timothy R.; Latham, David W.; Chaplin, William J.; Handberg, Rasmus; Huber, Daniel; Kipping, David M.; Payne, Matthew J.; Jiang, Chen; Victor Silva Aguirre; Stello, Dennis; Sliski, David H.; Ciardi, David R.; Buchhave, Lars A.; Bedding, Timothy R.; Davies, Guy R.; Hekker, Saskia; Kjeldsen, Hans; Everett, Mark E.; Howell, Steve B.; Basu, Sarbani; Campante, Tiago L.; Christensen-Dalsgaard, Jørgen; Elsworth, Yvonne P.; Karoff, Christoffer; Kawaler, Steven D.; Lund, Mikkel N.; Lundkvist, Mia; Esquerdo, Gilbert A.; et al. (2014). "Kepler-432: A red giant interacting with one of its two long period giant planets". The Astrophysical Journal. 803 (2): 49. arXiv: 1411.4666 . Bibcode:2015ApJ...803...49Q. doi:10.1088/0004-637X/803/2/49. S2CID   28994316.
  4. ↑ "Kepler-432". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-21.
  5. ↑ Morton, Timothy; Johnson, John (23 August 2011). "On the Low False Positive Probabilities of Kepler Planet Candidates". The Astrophysical Journal. 738 (2): 170. arXiv: 1101.5630 . Bibcode:2011ApJ...738..170M. doi:10.1088/0004-637X/738/2/170. S2CID   35223956.
  6. ↑ NASA (27 January 2014). "Kepler – Discoveries – Summary Table". NASA. Archived from the original on 27 May 2010. Retrieved 1 March 2014.
  7. 1 2 "Kepler Input Catalog search result". Space Telescope Science Institute . Retrieved 25 July 2015.
  8. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv: 1012.0707 [astro-ph.SR].
  9. ↑ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today . Retrieved 19 February 2011.
  10. ↑ Fraser Cain (September 15, 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
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