Epoch J2000.0 Equinox J2000.0
|Right ascension||10h 11m 22.14051s|
|Declination||+49° 27′ 15.2567″|
|Apparent magnitude (V)||+6.60|
|Spectral type||K7.5 Ve|
|U−B color index||+1.27|
|B−V color index||+1.34|
|Variable type||BY Dra, Flare star|
|Radial velocity (Rv)||–26.8 km/s|
|Proper motion (μ)||RA: –1362.32 mas/yr
Dec.: –504.52 mas/yr
|Parallax (π)||205.21 ± 0.54 mas|
|Distance||15.89 ± 0.04 ly
(4.87 ± 0.01 pc)
|Absolute magnitude (MV)||8.11|
|Luminosity (bolometric)||0.15 L☉|
|Luminosity (visual, LV)||0.046 L☉|
|Habitable zone inner limit||0.398[note 1] au|
|Habitable zone outer limit||0.755 au|
|Surface gravity (log g)||4.51; 4.70 cgs|
|Metallicity [Fe/H]||–0.03 dex|
|Rotational velocity (v sin i)||2.8 km/s|
Groombridge 1618 is a star in the northern constellation Ursa Major. With an apparent visual magnitude of +6.6, it lies at or below the threshold of stars visible to the naked eye for an average observer. It is located close to Earth, at a distance of less than 16 light years. This is a main sequence star of spectral type K7.5 Ve, having just 67% of the Sun's mass. There is a suspected planetary companion with an orbital period of 122 days.
This star was first identified as entry number 1618 in the work A Catalog of Circumpolar Stars, published posthumously by Stephen Groombridge in 1838. It has a high proper motion across the sky, which is normally taken as an indicator that the star is located nearby—making it an early candidate for parallax measurement of its distance. In 1884 the parallax angle was measured as 0″.322 ± 0″.023, which is larger than the modern value of 0″.205.
Groombridge 1618 has a stellar classification of K8 V, which means it is a K-type main sequence star that is generating energy by fusing hydrogen at its core. It has 67% of the mass of the Sun, 61% of the Sun's radius, but radiates only 15% of the Sun's energy and only 4.6% of the Sun's energy in the visible light spectrum. The effective surface temperature of the star's photosphere is about 4,000 K, giving it an orange hue.
It is a BY Draconis variable with a surface magnetic field strength of 750 G. The chromosphere is relatively inactive and possesses star spots comparable to Sun spots. However, like the star UV Ceti, it has been observed to undergo increases in luminosity as a flare star.
A search for an excess amount of infrared emission from this star by the Infrared Space Observatory came up negative, implying that Groombridge 1618 does not possess a debris disk (such as Vega). However, observations using the Herschel Space Observatory showed a small excess suggesting the presence of a low temperature debris disk. The data can be modeled by a ring of coarse, highly-reflective dust at a temperature below 22 K orbiting at least 51 AU from the host star. If this star does have a companion, astrometric measurements appear to place an upper bound of 3–12 times the mass of Jupiter on such a hypothetical object (for orbital periods in the range of 5–50 years).
According to Marcy & Benitz (1989), a possible periodicity of 122 days has been detected, inferring the potential presence of a massive planetary object with minimum mass 4 times that of Jupiter. This candidate planet has not been confirmed and the signal the authors had found could have been due to intrinsic stellar activity from the star's young age. If confirmed, the planet would be located within the star's habitable zone.[note 1]
(in order from star)
|b (unconfirmed)||≳4 MJ||0.41||122.5||0||—||—|
The habitable zone for this star, defined as the locations where liquid water could be present on an Earth-like planet, is at a radius of 0.26–0.56 AU, where 1 AU is the average distance from the Earth to the Sun.
-  when used to calculate the stellar flux reaching the outer atmosphere of an Earth-like planet orbiting Groombridge 1618 at the Inner Habitable Zone edge - the Runaway Greenhouse limit gives a of 0.9397 or 93.97% the stellar ﬂux reaching the top of Earth's atmosphere. By applying the previously calculated stellar flux and the known 15% luminosity of Groombridge 1618 into the equation, , the distance of the Inner HZ - Runaway Greenhouse limit from Groombridge 1618 can be calculated as .
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