Kepler-88

Last updated
Kepler-88
Observation data
Epoch J2000       Equinox J2000
Constellation Lyra
Right ascension 19h 24m 35.54310s [1]
Declination +40° 40′ 09.8099″ [1]
Apparent magnitude  (V)13.257 [2]
Characteristics
Spectral type G6V [3]
Astrometry
Radial velocity (Rv)−19.51±1.63 [1]  km/s
Proper motion (μ)RA: 1.150(11)  mas/yr [1]
Dec.: 4.956(15)  mas/yr [1]
Parallax (π)2.6495 ± 0.0109  mas [1]
Distance 1,231 ± 5  ly
(377 ± 2  pc)
Absolute magnitude  (MV)5.46±0.16 [4]
Details
Mass 0.990±0.023 [5]   M☉
Radius 0.897±0.016 [5]   R☉
Luminosity 0.598+0.079
−0.070 [4]   L☉
Surface gravity (log g)4.528+0.025
−0.019 [4]   cgs
Temperature 5466±60 [5]   K
Metallicity [Fe/H]+0.27±0.06 [5]   dex
Rotation 30.689±0.383 days [6]
Age 1.9±1.6 [5]   Gyr
Other designations
Kepler-88, KOI-142, KIC  5446285, TIC  122712595, 2MASS J19243554+4040098 [2]
Database references
SIMBAD data
KIC data

Kepler-88 is a G-type star 1,230 light-years (380 parsecs ) away in the constellation of Lyra, with three confirmed exoplanets. [5] SIMBAD lists a subgiant spectral type of G8IV, [2] while other sources give it a main sequence spectral type of G6V. [3] The latter is more consistent with its properties (it is less luminous than the Sun).

Planetary system

In April 2012, scientists discovered that a Kepler candidate known as KOI-142.01 (Kepler-88b) exhibited very significant transit-timing variations caused by a non-transiting planet. [4] The timing variations were large enough to cause changes to the transit durations of Kepler-88b as well. Large transit-timing variations helped to put tight constraints on the masses of both planets. The non-transiting planet, Kepler-88c, was further confirmed through the radial velocity method in November 2013. [3]

Kepler-88b is the innermost planet in the system and is Neptune-sized but almost half as massive. Kepler 88c is about 67% as massive as Jupiter, but its radius is not known due to not transiting the star. [5]

Kepler-88d orbits its star every four years, and its orbit is not circular, but elliptical. At three times the mass of Jupiter, it is the most massive planet known in the system. It was discovered based on six years of radial velocity (RV) follow-up from the W. M. Keck Observatory HIRES spectrograph. [5]

The Kepler-88 planetary system [5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b9.5±1.1  M🜨 0.09810.91647±0.000140.05561±0.0001390.97±0.12 ° 3.438±0.075  R🜨
c0.674±0.016  MJ 0.1552522.26492±0.000670.05724±0.0004593.15±0.68 ° —
d≥3.05±0.16  MJ 2.45±0.021403±140.41±0.03——

Related Research Articles

<span class="mw-page-title-main">Kepler-9</span> Star located in the constellation Lyra

Kepler-9 is a sunlike star in the constellation Lyra. Its planetary system, discovered by the Kepler Mission in 2010 was the first detected with the transit method found to contain multiple planets.

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.

Kepler-39 is an F-type main sequence star located in the constellation Cygnus. It is located about 3,560 light-years away. One known substellar companion orbits it, Kepler-39b.

Kepler-19 is a G7V star that is host to three known planets - Kepler-19b, Kepler-19c, and Kepler-19d. It is located about 720 light-years away in the constellation Lyra, five arcminutes northwest of the much more distant open cluster NGC 6791.

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

<span class="mw-page-title-main">Kepler-19c</span> Neptunian planet orbiting Kepler-19

Kepler-19c is an extra-solar planet orbiting the star Kepler-19 approximately 717 light years from Earth.

<span class="mw-page-title-main">Kepler-46</span> Old star with a planetary system

Kepler-46, previously designated KOI-872, is a star located in the constellation Lyra. Observed since 2009 by the Kepler space observatory, it has since been found to possess a planetary system consisting of at least three planets and while it has a similar mass to the Sun (90%) it is significantly older at ten billion years.

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-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.

Kepler-89 is a star with four confirmed planets. Kepler-89 is a possible wide binary star.

Kepler-65 is a subgiant star slightly more massive than the Sun and has at least four planets.

Kepler-66 is a star with slightly more mass than the Sun in the NGC 6811 open cluster in the Cygnus constellation. It has one confirmed planet, slightly smaller than Neptune, announced in 2013.

<span class="mw-page-title-main">Hunt for Exomoons with Kepler</span> Space research project

The Hunt for Exomoons with Kepler (HEK) is a project whose aim is to search for exomoons, natural satellites of exoplanets, using data collected by the Kepler space telescope. Founded by British exomoonologist David Kipping and affiliated with the Center for Astrophysics | Harvard & Smithsonian, HEK submitted its first paper on June 30, 2011. HEK has since submitted five more papers, finding some evidence for an exomoon around a planet orbiting Kepler-1625b in July 2017.

<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-43, formerly known as KOI-135, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 00m 57.8034s, Declination +46° 40′ 05.665″. With an apparent visual magnitude of 13.996, this star is too faint to be seen with the naked eye. The Kepler-43 has a very strong starspot activity.

Kepler-1625 is a 14th-magnitude solar-mass star located in the constellation of Cygnus approximately 7,200 light-years away. Its mass is within 5% of that of the Sun, but its radius is approximately 70% larger reflecting its more evolved state. A candidate gas giant exoplanet was detected by the Kepler Mission around the star in 2015, which was later validated as a real planet to >99% confidence in 2016. In 2018, the Hunt for Exomoons with Kepler project reported evidence for a Neptune-sized exomoon around this planet, based on observations from NASA’s Kepler mission and the Hubble Space Telescope. Subsequently, the evidence for and reality of this exomoon candidate has been subject to debate.

Kepler-1625b is a super-Jupiter exoplanet orbiting the Sun-like star Kepler-1625 about 2,500 parsecs away in the constellation of Cygnus. The large gas giant is approximately the same radius as Jupiter, and orbits its star every 287.4 days. In 2017, hints of a Neptune-sized exomoon in orbit of the planet was found using photometric observations collected by the Kepler Mission. Further evidence for a Neptunian moon was found the following year using the Hubble Space Telescope, where two independent lines of evidence constrained the mass and radius to be Neptune-like. The mass-signature has been independently recovered by two other teams. However, the radius-signature was independently recovered by one of the teams but not the other. The original discovery team later showed that this latter study appears affected by systematic error sources that may influence their findings.

Kepler-51 is a Sun-like star that is about 500 million years old. It is orbited by three super-puff planets—Kepler-51b, c, and d—which have the lowest known densities of any known exoplanet. The planets are similar in radius to gas giants like Jupiter, but have unusually small masses for their size, only a few times greater than Earth’s.

References

  1. 1 2 3 4 5 6 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 "Kepler-88". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 19 February 2024.
  3. 1 2 3 Barros, S. C. C.; Díaz, R. F.; et al. (January 2014). "SOPHIE velocimetry of Kepler transit candidates. X. KOI-142 c: first radial velocity confirmation of a non-transiting exoplanet discovered by transit timing". Astronomy & Astrophysics . 561: L1. arXiv: 1311.4335 . Bibcode:2014A&A...561L...1B. doi:10.1051/0004-6361/201323067.
  4. 1 2 3 4 Nesvorný, David; Kipping, David; Terrell, Dirk; Hartman, Joel; Bakos, Gáspár Á; Buchhave, Lars A (2013). "KOI-142, the King of Transit Variations, is a Pair of Planets Near the 2:1 Resonance". The Astrophysical Journal. 777 (1): 3. arXiv: 1304.4283 . Bibcode:2013ApJ...777....3N. doi:10.1088/0004-637X/777/1/3. S2CID   59933168.
  5. 1 2 3 4 5 6 7 8 9 Weiss, Lauren M.; Fabrycky, Daniel C.; Agol, Eric; Mills, Sean M.; Howard, Andrew W.; Isaacson, Howard; Petigura, Erik A.; Fulton, Benjamin; Hirsch, Lea; Sinukoff, Evan (2020-04-29). "The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis" (PDF). The Astronomical Journal. 159 (5): 242. arXiv: 1909.02427 . Bibcode:2020AJ....159..242W. doi: 10.3847/1538-3881/ab88ca . ISSN   1538-3881. S2CID   202539420.
  6. ↑ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1): L11. arXiv: 1308.1845 . Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID   118557681.
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