Kepler-13

Last updated
Kepler-13
Observation data
Epoch J2000       Equinox J2000
Constellation Lyra [1]
Kepler-13 A
Right ascension 19h 07m 53.1397s [2]
Declination 46° 52′ 05.922″ [2]
Apparent magnitude  (V)9.95 [3]
Kepler-13 B
Right ascension 19h 07m 53.0281s [4]
Declination 46° 52′ 06.126″ [4]
Apparent magnitude  (V)10.33 [5]
Characteristics
Spectral type A0
Variable type Planetary transit variable [6]
Astrometry
Kepler-13 A
Proper motion (μ)RA: −4.411(42)  mas/yr [2]
Dec.: −15.220(50)  mas/yr [2]
Parallax (π)2.0319 ± 0.0344  mas [2]
Distance 1,610 ± 30  ly
(492 ± 8  pc)
Kepler-13 B
Proper motion (μ)RA: −4.060(33)  mas/yr [4]
Dec.: −15.512(40)  mas/yr [4]
Parallax (π)2.0912 ± 0.0263  mas [4]
Distance 1,560 ± 20  ly
(478 ± 6  pc)
Details [7]
Kepler-13A
Mass 1.72±0.10  M☉
Radius 1.71±0.04  R☉
Surface gravity (log g)4.2±0.5  cgs
Temperature 7650±250  K
Metallicity [Fe/H]0.2±0.2  dex
Rotational velocity (v sin i)78±15 km/s
Age 0.5±0.1  Gyr
Kepler-13B
Mass 1.68±0.10  M☉
Radius 1.68±0.04  R☉
Surface gravity (log g)4.2±0.5  cgs
Temperature 7530±250  K
Metallicity [Fe/H]0.2±0.2  dex
Rotational velocity (v sin i)69±13 km/s
Age 0.5±0.1  Gyr
Other designations
BD+46 2629, ADS  12085 AB, WDS J19079+4652AB, KOI-13, KIC  9941662, 2MASS J19075308+4652061 [3]
Database references
SIMBAD data

Kepler-13 or KOI-13 is a stellar triple star system consisting of Kepler-13A, around which an orbiting hot Jupiter exoplanet was discovered with the Kepler spacecraft in 2011, and Kepler-13B a common proper motion companion star which has an additional star orbiting it. [8]

Contents

Stellar system

The multiple nature of the system was discovered in 1904 by Robert Grant Aitken at Lick Observatory. He measured a separation between the A and B components of approximately one arc second and position angle of 281.3° with the 36" James Lick telescope. [9] The position of the two visual components of the system relative to each other has remained constant since 1904. [10] Radial velocity measurements taken with the SOPHIE échelle spectrograph at the Haute-Provence Observatory revealed an additional companion orbiting Kepler-13B. This companion has a mass of between 0.4 and 1 times that of the Sun and orbits with a period of 65.831 days with an eccentricity of 0.52 [8]

Planetary system

Kepler-13 was identified as one of 1235 planetary candidates with transit-like signatures in the first four months of Kepler data. [11] It was confirmed as a planet by measuring the Doppler beaming effect on the Kepler light curve. [6] The planet that has been confirmed, having a radius of between 1.5 and 2.6 RJ, is also one of the largest known exoplanets.

The planet is likely to be tidally locked to the parent star. In 2015, the planetary nightside temperature was estimated to be equal to 2394±251 K. [12]

The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is mildly misaligned with the equatorial plane of the star, misalignment equal to 24±4°. [13]

The planetary transits are changing in duration over time which is likely caused by the interaction of the planet with its host star. [14] [15]

In 2017, it was revealed that titanium monoxide molecules in the dayside might be carried to the nightside of the planet, where they form clouds and precipitate. [16]

The Kepler-13 planetary system [17]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b9.28(16)  MJ 0.03641(87)1.763588(1)0.00064+0.00012
−0.00016		86.770+0.048
−0.052 ° 		2.216(87)  RJ

Related Research Articles

<span class="mw-page-title-main">Kepler-4b</span> Extrasolar planet in the constellation Draco

Kepler-4b, initially known as KOI 7.01, is an extrasolar planet first detected as a transit by the Kepler spacecraft. Its radius and mass are similar to that of Neptune; however, due to its proximity to its host star, it is substantially hotter than any planet in the Solar System. The planet's discovery was announced on January 4, 2010, in Washington, D.C., along with four other planets that were initially detected by the Kepler spacecraft and subsequently confirmed by telescopes at the W.M. Keck Observatory.

Kepler-18 is a star with almost the same mass as the Sun in the Cygnus constellation.

Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V. This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the main sequence. Kepler-80, like other red dwarf stars, is smaller than the Sun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star. Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.

Kepler-68 is a Sun-like main sequence star located 471 light-years away in the constellation Cygnus. It is known to have at least four planets orbiting around it. The third planet has a mass similar to Jupiter but orbits within the habitable zone.

Kepler-32 is an M-type main sequence star located about 1070 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, it shows a 0.58 ± 0.05 solar mass (M☉), a 0.53 ± 0.04 solar radius (R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity.

<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-56</span> Red giant star in the constellation Cygnus

Kepler-56 is a red giant in constellation Cygnus roughly 3,060 light-years (940 pc) away with slightly more mass than the Sun.

<span class="mw-page-title-main">Kepler-25</span> Yellow-white hued star in the constellation Lyra

Kepler-25 is a star in the northern constellation of Lyra. It is slightly larger and more massive than the Sun, with a luminosity 21⁄2 times that of the Sun. With an apparent visual magnitude of 10.6, this star is too faint to be seen with the naked eye.

Kepler-102 is a star 353 light-years away in the constellation of Lyra. Kepler-102 is less luminous than the Sun. The star system does not contain any observable amount of dust. Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU.

<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-30 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 19h 01m 08.0747s Declination +38° 56′ 50.219″. With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye. Kepler-30 is exhibiting a strong starspot activity.

Kepler-29 is a Sun-like star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 53m 23.6020s, Declination +47° 29′ 28.436″. With an apparent visual magnitude of 15.456, this star is too faint to be seen with the naked eye. It is a solar analog, having a close mass, radius, and temperature as the Sun. Currently the age of the star has not been determined due to its 2780 light-year distance. As of 2016 no Jovian exoplanets of 0.9–1.4 MJ have been found at a distance of 5 AU.

<span class="mw-page-title-main">Kepler-444</span> Triple star system in the constellation of Lyra

Kepler-444 is a triple star system, estimated to be 11.2 billion years old, approximately 119 light-years (36 pc) away from Earth in the constellation Lyra. On 27 January 2015, the Kepler spacecraft is reported to have confirmed the detection of five sub-Earth-sized rocky exoplanets orbiting the main star. The star is a K-type main sequence star. All of the planets are far too close to their star to harbour life forms.

Kepler-296 is a binary star system in the constellation Draco. The primary star appears to be a late K-type main-sequence star, while the secondary is a red dwarf.

<span class="mw-page-title-main">KOI-256</span> Double star in the constellation Cygnus

KOI-256 is a double star located in the constellation Cygnus approximately 575 light-years (176 pc) from Earth. While observations by the Kepler spacecraft suggested the system contained a gas giant exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf.

<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-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.

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 "Kepler-13". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-01-07.
  4. 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.
  5. ↑ Howarth, Ian D.; Morello, Giuseppe (2017). "Rapid rotators revisited: Absolute dimensions of KOI-13". Monthly Notices of the Royal Astronomical Society. 470 (1): 932–939. arXiv: 1705.07302 . Bibcode: 2017MNRAS.470..932H . doi: 10.1093/mnras/stx1260 . S2CID   31123194.
  6. 1 2 Shporer, Avi; et al. (2011). "Detection of Koi-13.01 Using the Photometric Orbit". The Astronomical Journal. 142 (6) 195. arXiv: 1110.3510 . Bibcode: 2011AJ....142..195S . doi: 10.1088/0004-6256/142/6/195 .
  7. ↑ Shporer, Avi; et al. (2014). "Atmospheric Characterization of the Hot Jupiter Kepler-13Ab". The Astrophysical Journal. 788 (1) 92. arXiv: 1403.6831 . Bibcode:2014ApJ...788...92S. doi: 10.1088/0004-637X/788/1/92 .
  8. 1 2 Santerne, A.; et al. (2012). "SOPHIE velocimetry of Kepler transit candidates. VI. An additional companion in the KOI-13 system". Astronomy and Astrophysics. 544 L12. arXiv: 1207.1715 . Bibcode: 2012A&A...544L..12S . doi: 10.1051/0004-6361/201219899 . S2CID   118482346.
  9. ↑ Aitken, Robert Grant (1904). "Measures of one hundred fifty-five new double stars". Lick Observatory Bulletin. 3: 6–18. Bibcode: 1904LicOB...3....6A . doi:10.5479/ADS/bib/1904LicOB.3.6A.
  10. ↑ Szabó, Gy. M.; et al. (2011). "Asymmetric Transit Curves As Indication of Orbital Obliquity: Clues from the Late-Type Dwarf Companion in Koi-13". The Astrophysical Journal Letters. 736 (1) L4. arXiv: 1105.2524 . Bibcode: 2011ApJ...736L...4S . doi: 10.1088/2041-8205/736/1/L4 .
  11. ↑ 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 .
  12. ↑ Angerhausen, Daniel; et al. (2015). "A Comprehensive Study of Kepler Phase Curves and Secondary Eclipses: Temperatures and Albedos of Confirmed Kepler Giant Planets". Publications of the Astronomical Society of the Pacific. 127 (957): 1113–1130. arXiv: 1404.4348 . Bibcode: 2015PASP..127.1113A . doi: 10.1086/683797 .
  13. ↑ Albrecht, Simon; et al. (2012). "Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments". The Astrophysical Journal. 757 (1) 18. arXiv: 1206.6105 . Bibcode: 2012ApJ...757...18A . doi: 10.1088/0004-637X/757/1/18 .
  14. ↑ Szabó, Gy. M.; et al. (2011). "Spin-orbit resonance, transit duration variation and possible secular perturbations in KOI-13". MNRAS. 421 (1) L122. arXiv: 1110.4231 . Bibcode: 2012MNRAS.421L.122S . doi: 10.1111/j.1745-3933.2012.01219.x .
  15. ↑ Shahaf, Sahar; et al. (12 May 2021). "Systematic search for long-term transit duration changes in Kepler transiting planets". Monthly Notices of the Royal Astronomical Society. 505 (1): 1293–1310. arXiv: 2105.04318 . Bibcode: 2021MNRAS.505.1293S . doi: 10.1093/mnras/stab1359 .
  16. ↑ "Hubble Observes Exoplanet that Snows Sunscreen - NASA Science". science.nasa.gov. Retrieved 2024-01-06.
  17. ↑ Esteves, Lisa J.; Mooij, Ernst J. W. De; Jayawardhana, Ray (2015). "Changing Phases of Alien Worlds: Probing Atmospheres Of Kepler planets with High-Precision Photometry". The Astrophysical Journal. 804 (2) 150. arXiv: 1407.2245 . Bibcode: 2015ApJ...804..150E . doi: 10.1088/0004-637X/804/2/150 .
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