Kepler-88

{{Starbox observe

| epoch = J2000

| constell = Lyra

| ra = {{RA|19|24|35.54310}}

| dec = {{DEC|+40|40|09.8099}}

| appmag_v = 13.257

}}

{{Starbox character

| class = G6V

}}

{{Starbox astrometry

| radial_v = {{val|-19.51|1.63}}

| prop_mo_ra = {{val|1.150|(11)}}

| prop_mo_dec = {{val|4.956|(15)}}

| pm_footnote =

| parallax = 2.6495

| p_error = 0.0109

| parallax_footnote =

| absmag_v = {{val|5.46|0.16}}

}}

{{Starbox detail

| mass = {{val|0.990|0.023}}

| radius = {{val|0.897|0.016}}

| luminosity = {{val|0.598|0.079|0.070}}

| gravity = {{val|4.528|0.025|0.019}}

| temperature = {{val|5466|60}}

| metal_fe = {{val|+0.27|0.06}}

| rotation = {{val|30.689|0.383|s= days}}

| age_gyr = {{val|1.9|1.6}}

}}

{{Starbox catalog

| names = {{odlist | 2MASS=J19243554+4040098 | Kepler=88 | KIC=5446285 | KOI=142 | TIC=122712595}}

}}

{{Starbox reference

| Simbad = Kepler-88

| KIC = 5446285

}}

Kepler-88 is a G-type star {{convert|1230|ly|pc|lk=on|abbr=off}} away in the constellation of Lyra, with three confirmed exoplanets. SIMBAD lists a subgiant spectral type of G8IV, while other sources give it a main sequence spectral type of G6V. 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. 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.

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.

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.

{{OrbitboxPlanet begin

| name = Kepler-88

| table_ref =

}}

{{OrbitboxPlanet

| exoplanet = b

| mass_earth = {{val|9.5|1.1}}

| period = {{val|10.91647|0.00014}}

| semimajor = 0.098

| eccentricity = {{val|0.05561|0.00013}}

| inclination = {{val|90.97|0.12}}

| radius_earth = {{val|3.438|0.075}}

}}

{{OrbitboxPlanet

| exoplanet = c

| mass = {{val|0.674|0.016}}

| period = {{val|22.26492|0.00067}}

| semimajor = 0.15525

| eccentricity = {{val|0.05724|0.00045}}

| inclination = {{val|93.15|0.68}}

| radius =

}}

{{OrbitboxPlanet

| exoplanet = d

| mass = {{val|3.05|0.16|p=≥}}

| period = {{val|1403|14}}

| semimajor = {{val|2.45|0.02}}

| eccentricity = {{val|0.41|0.03}}

}}

References

{{reflist|refs=

{{cite journal|bibcode=2013ApJ...777....3N|doi=10.1088/0004-637X/777/1/3|arxiv=1304.4283|title=KOI-142, the King of Transit Variations, is a Pair of Planets Near the 2:1 Resonance|journal=The Astrophysical Journal|volume=777|issue=1|pages=3|year=2013|last1=Nesvorný|first1=David|last2=Kipping|first2=David|last3=Terrell|first3=Dirk|last4=Hartman|first4=Joel|last5=Bakos|first5=Gáspár Á|last6=Buchhave|first6=Lars A|s2cid=59933168}}

{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | pages=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 | s2cid=118557681 }}

{{cite journal |last1=Barros |first1=S. C. C. |last2=Díaz |first2=R. F. |last3=Santerne |first3=A. |last4=Bruno |first4=G. |last5=Deleuil |first5=M. |last6=Almenara |first6=J.-M. |last7=Bonomo |first7=A. S. |last8=Bouchy |first8=F. |last9=Damiani |first9=C. |last10=Hébrard |first10=G. |last11=Montagnier |first11=G. |last12=Moutou |first12=C. |display-authors=2 |date=January 2014 |title=SOPHIE velocimetry of Kepler transit candidates. X. KOI-142 c: first radial velocity confirmation of a non-transiting exoplanet discovered by transit timing |journal=Astronomy & Astrophysics |volume=561 |issue= |pages=L1 |doi=10.1051/0004-6361/201323067 |arxiv=1311.4335 |bibcode=2014A&A...561L...1B}}

{{Cite journal|last1=Weiss|first1=Lauren M.|last2=Fabrycky|first2=Daniel C.|last3=Agol|first3=Eric|last4=Mills|first4=Sean M.|last5=Howard|first5=Andrew W.|last6=Isaacson|first6=Howard|last7=Petigura|first7=Erik A.|last8=Fulton|first8=Benjamin|last9=Hirsch|first9=Lea|last10=Sinukoff|first10=Evan|date=2020-04-29|title=The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis|journal=The Astronomical Journal|volume=159|issue=5|pages=242|doi=10.3847/1538-3881/ab88ca|arxiv=1909.02427|bibcode=2020AJ....159..242W|s2cid=202539420|issn=1538-3881|url=https://authors.library.caltech.edu/99954/1/1909.02427.pdf |doi-access=free }}

}}

Category:Planetary systems with three confirmed planets

142

Category:Lyra

J19243554+4040098

Category:Planetary transit variables

Category:G-type main-sequence stars