Mass
9.40e-3 Msun
9.40e-3 to 0.07
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Stellar HostProfile
MOA-2015-BLG-337L
Unclassified star โข 7100 pc
Records
4
literature rows
Planets
1
system count
References
2
distinct source labels
Approximate color
from effective temperature
Canonical Summary
Adopted host values from one source row
Values come from the row with the most populated summary measurements. Missing values stay missing. Ranges and counts describe all source rows.
Stellar source: Miyazaki et al. 2018 โข System source: Miyazaki et al. 2018
Distance
7100 pc
6300 to 7100
Planets
1
Stable across source rows
System Layout
Known planets
1 planets linked to this host
MOA-2015-BLG-337L b
Microlensing
โ
Discovery
2018
Period
โ
Radius
โ
Mass
33.70 Mโ
Eq. Temp
โ
MOA-2015-BLG-337L b: A Microlensing World Around a Tiny Star
MOA-2015-BLG-337L is a host star 23,200 light-years away with a reported mass of 0.0094 solar masses, an estimate smaller than the Sun's mass. One planet is known to orbit it.
That planet, MOA-2015-BLG-337L b, was discovered in 2018 by microlensing, a method that reveals a planet through the way its gravity briefly brightens a background star. Its reported mass is 33.7 Earth masses, larger than Earth's mass.
No orbital period is reported for MOA-2015-BLG-337L b, so its year remains unmeasured. The star's low mass, paired with the planet's comparatively large mass, makes this a striking system: a world of 33.7 Earth masses circling a star of only 0.0094 solar masses.
Provenance
Underlying measurements and references
Evidence Summary
Rows
4
Stellar refs
1
System refs
1
Distancedisputed
Massdisputed
| ST TEFF | ST MASS | ST RAD | ST AGE | ST LUM | ST SPECTYPE | SY DIST | Stellar Ref | System Ref |
|---|---|---|---|---|---|---|---|---|
| โ | 9.40e-3 | โ | โ | โ | โ | 7100 | Miyazaki et al. 2018 | Miyazaki et al. 2018 |
| โ | 9.40e-3 | โ | โ | โ | โ | 7100 | Miyazaki et al. 2018 | Miyazaki et al. 2018 |
| โ | 0.07 | โ | โ | โ | โ | 6300 | Miyazaki et al. 2018 | Miyazaki et al. 2018 |
| โ | 0.07 | โ | โ | โ | โ | 6300 | Miyazaki et al. 2018 | Miyazaki et al. 2018 |