Temperature
6030 K
5460 to 6178
F9 IV • 685.2 pc
Records
7
literature rows
Planets
1
system count
References
8
distinct source labels
Approximate color
from effective temperature
Canonical Summary
Values come from the row with the most populated summary measurements. Missing values stay missing. Ranges and counts describe all source rows.
Stellar source: Eigmüller et al. 2017 • System source: TICv8
Temperature
6030 K
5460 to 6178
Mass
1.30 Msun
1.11 to 1.30
Radius
1.78 Rsun
1.33 to 1.91
Age
4.25 Gyr
single adopted value
Distance
685.2 pc
single adopted value
Spectral Type
F9 IV
Consistent across records
Planets
1
Stable across source rows
Scale Comparison
Current adopted radius: 1.78 R☉ (circles scaled linearly by radius)
Sun
1.0 R☉ baseline
K2-107
1.78 R☉
System Layout
1 planets linked to this host
Transit
Discovery
2017
Period
3.31 days
Radius
15.98 R⊕
Mass
—
Eq. Temp
1649 K
K2-107 is a star 2230 light-years away with a spectral type of F9 IV. It is 4.25 billion years old and has 1.3 solar masses, 1.78 solar radii, and a temperature of 6030 K. Its reported mass estimate is larger than the Sun's, its reported radius estimate is larger than the Sun's, and its reported temperature is hotter than the Sun's. One planet orbits this host.
K2-107 b is a Jupiter-like planet discovered by transit in 2017. Its radius is 16 Earth radii, larger than Earth's, and its orbital period is 3.31 days.
Provenance
Evidence Summary
Rows
7
Stellar refs
7
System refs
1
| ST TEFF | ST MASS | ST RAD | ST AGE | ST LUM | ST SPECTYPE | SY DIST | Stellar Ref | System Ref |
|---|---|---|---|---|---|---|---|---|
| — | — | 1.91 | — | — | — | 685.2 | Kruse et al. 2019 | TICv8 |
| 6178 | 1.26 | 1.33 | — | — | — | 685.2 | Mayo et al. 2018 | TICv8 |
| — | — | 1.73 | — | — | — | 685.2 | Petigura et al. 2018 | TICv8 |
| 6001 | 1.11 | 1.80 | — | 0.58 | — | 685.2 | TICv8 | TICv8 |
| 6061 | 1.30 | 1.81 | — | — | — | 685.2 | Livingston et al. 2018 | TICv8 |
| 5460 | — | 1.91 | — | 0.46 | — | 685.2 | Gaia DR2 | TICv8 |
| 6030 | 1.30 | 1.78 | 4.25 | — | F9 IV | 685.2 | Eigmüller et al. 2017 | TICv8 |