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Stellar HostProfile

Oph 11

M9

Records

3

literature rows

Planets

1

system count

References

4

distinct source labels

TIC: TIC 392045047

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: Close et al. 2007 • System source: TICv8

Temperature

2375 K

2375 to 2878

2 values • 2 distinct

Mass

0.02 Msun

0.02 to 0.20

3 values • 3 distinct

Age

5 Gyr

0.01 to 5

2 values • 2 distinct

Luminosity

-2.77 log(Lsun)

-2.77 to -2.48

2 values • 2 distinct

Spectral Type

M9

Consistent across records

M9 (1)

Planets

1

Stable across source rows

1

System Layout

Known planets

1 planets linked to this host

Oph 11 b

Imaging

◌

Discovery

2006

Period

7300000 days

Radius

—

Mass

4449.6 M⊕

Eq. Temp

2175 K

Oph 11 and Its Imaged Companion

Oph 11 is an M9 host star, placing it among the small, cool red dwarfs. Its spectral class is cooler than the Sun's, and its reported temperature is 2380 K. The star's reported mass estimate is 0.016 solar masses, smaller than the Sun's, and its age is 5 billion years. One planet orbits this host.

That planet is Oph 11 b, discovered by imaging in 2006. It has a reported mass estimate of 4450 Earth masses, larger than Earth's and roughly 14 times Jupiter's mass. Its orbital period is 7300000 days.

Provenance

Underlying measurements and references

Evidence Summary

Rows

3

Stellar refs

3

System refs

1

Temperaturedisputed

2 values • 2 distinct

Massdisputed

3 values • 3 distinct

Radiusstable

1 values • 1 distinct

Agedisputed

2 values • 2 distinct

Luminositydisputed

2 values • 2 distinct

Surface Gravitydisputed

2 values • 2 distinct

Spectral Typestable

1 values • 1 distinct

ST TEFFST MASSST RADST AGEST LUMST SPECTYPESY DISTStellar RefSystem Ref
—0.05—0.01———Pecaut et al. 2012TICv8
28780.200.23—-2.48——TICv8TICv8
23750.02—5-2.77M9—Close et al. 2007TICv8