Kepler-90g

{{Short description|Super-puff exoplanet in the constellation Draco}}

{{Infobox planet

| extrasolarplanet = yes

| name = Kepler-90g

| image =

| image_size =

| image_alt =

| caption =

| apsis = astron

| discovery_ref =

| discoverer = Cabrera et al.

| discovery_site =

| discovered = October 2013

| discovery_method = Transit

| alt_names = KOI-351 g, KOI-351.02

| periastron =

| apoastron =

| semimajor = {{val|0.71|0.08}} AU

| avg_speed =

| eccentricity = {{val|0.049|0.011|0.007}}

| period = {{val|210.48|0.05|0.05|ul=d}}

| inclination = {{val|89.92|0.03|0.01|ul=deg}}

| angular_dist =

| arg_peri = {{val|90|20|20|ul=deg}}

| time_periastron =

| semi-amplitude =

| star = Kepler-90

| mean_radius = {{val|8.1|0.8|ul=Earth radius}}

| surface_area =

| volume =

| density = {{val|0.15|0.05|ul=g/cm3}}

| mass = {{val|15.0|0.9|0.8|ul=Earth mass}}

| surface_grav =

| moment_of_inertia_factor =

| escape_velocity =

| albedo =

| single_temperature = {{convert|349|K|C}}

}}

Kepler-90g (also known by its Kepler Object of Interest designation KOI-351.02) is a super-puff exoplanet orbiting the early G-type main sequence star Kepler-90, one of eight planets around this star discovered using NASA's Kepler space telescope. It is located about {{convert|2840|ly|pc}} from Earth,{{cite DR2|2132193431285570304}} in the constellation Draco. 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. It orbits its parent star about every 210.5 days at a distance of 0.71 astronomical units.

Kepler-90g's orbital period changes by 25.7 hours between two consecutive transits, caused by gravitational perturbations from other planets in the system. Additionally, changes in the depth and duration of transit events led to an exomoon being hypothesized to orbit this planet. However, this candidate moon was later found to be a false positive.

A 2020 analysis of transit-timing variations of Kepler-90g and h found a best-fit mass of {{val|15|0.9|0.8|ul=Earth mass}} for planet g. This is between the masses of Uranus and Neptune. Given a transit-derived radius of {{val|8.1|ul=Earth radius}}, Kepler-90g was found to have an extremely low density of {{val|0.15|0.05|ul=g/cm3}}, unusually inflated for its mass and insolation. Several possible explanations for its apparently low density include a puffy planet with a dusty atmosphere or a smaller planet surrounded by a tilted wide ring system (albeit the latter option is less likely due to the lack of evidence for rings in transit data).

File:Kepler-90 system rightward-PIA22193.jpg