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Stellar Catalog
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Nearby stars catalogue
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G 182-34
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Star G 182-34

Red dwarf G 182-34 is located 98 light years away from the Sun. It is a single star of spectral class M3.5Ve, that has 37 % of solar mass. There is at least one exoplanet in this system.
Sun distance
98 light years

G 182-34

Red dwarf (spectral class M3.5Ve)

Location

Ascension iconRight ascension: 18h 1m 16.141s
Declination iconDeclination: 35° 35' 41.351'' (northern hemisphere)
Parallax iconParallax: 33.264
Distance iconSun distance: 98.05 ly | 30.1 pc

Basic characteristic

icon weight
Mass: 36.8 % M Sun | 386 M Jupiter
radius icon
Size: 37 % R Sun | 3.7 R Jupiter
temperature iconTemperature: 3422 K | 0.59 T Sun
time iconAge: 5.1 billions years | 1.11 Sun
luminosity iconLuminosity: 0.01706 L Sun

1 exoplanet

G 182-34 b 0.05 AU 5.4 M 2.5 R 7.4 days

Photometry

5
10
15
20
25
30
35
K
2.1
H
1.6
J
1.2
Grp
0.8
I
0.8
G
0.6
V
0.5
Gbp
0.5
B
0.4
U
0.3
Absolute stellar magnitude in different parts of the electromagnetic spectrum from infrared (K band) to ultraviolet (U band).
More about G 182-34
Nearby star G 182-34 is a main sequence star that fuses hydrogen atoms into helium. It is approximately 40 % of the size of Sun and temperature on its surface is around 3422 K (3149 °C), which is about 59 % of Sun's temperature.
      G 182-34 can be found in northern celestial hemisphere, however it is too dim to be seen with the naked eye or even a small telescope. 
Other designations of this star
TOI 4438, Karmn J18012+355, TIC 22233480, Gaia DR3 4606416269652179328
External sources
simbad icon
Simbad database (G 182-34)
Astronomical database SIMBAD (the Set of Identifications, Measurements and Bibliography for Astronomical Data)
gaia icon
Gaia database (Gaia DR3 4606416269652179328)
Archive from the Gaia mission
tess icon
TESS database (TOI 4438.01)
Archive from the TESS mission
Class of stars Red dwarf
Red dwarfs are small reddish stars, that are by far the most common type of star in solar neighborhood. Their mass is usually between 10 and 50 % of solar mass.
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