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GQ Lupi b
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GQ Lupi b
GQ Lupi b, or GQ Lupi B is a substellar companion to the T Tauri star GQ Lupi. Classified as either an exoplanet or a brown dwarf, this object is still in the early stages of its formation, accreting gas from its circumplanetary disk. GQ Lupi b is orbiting at nearly 100 astronomical units from the star, with an estimated orbital period around a millennium. The object was discovered by R. Neuhäuser et al., through direct imaging and announced in April 2005, less than a month before the full confirmation of 2M1207b was announced. Along with 2M1207b, this was one of the first extrasolar planet candidates to be directly imaged.
GQ Lupi b was discovered in 2005 by a team led by R. Neuhäuser. By analysing data taken from the NACO adaptive optics aboard the Very Large Telescope, they discovered a faint companion to GQ Lupi A, and combining this with archival observations from the Subaru and Hubble Space Telescopes, they were able to confirm that the companion co-moves with the star and thus is gravitationally bound. At the time, this was considered to be the first direct imaging discovery of a planetary-mass companion orbiting a star. The image was made with the European Southern Observatory's VLT telescope at the Paranal Observatory, Chile on June 25, 2004. In 2006, the IAU's Working Group on Extrasolar Planets described GQ Lup b as a "possible planetary-mass companion to a young star".
GQ Lupi b is within the Lupus I molecular cloud, a star-forming region that is part of the Scorpius–Centaurus association. The cloud is located at a distance of roughly 460 ± 160 light-years (140 ± 50 parsecs). The GQ Lupi system is located at a distance of 501.7+2.2
−2.7 ly (153.82+0.67
−0.82 pc). As seen from Earth, it is within the constellation of Lupus.
GQ Lupi b orbits at a semi-major axis of 98 astronomical units from its host star, having a moderate orbital eccentricity of 0.35. This means that the farthest passage (apoastron) occurs at 132 au while the closest passage (periastron) occurs at 64 au. The orbital period is of roughly 920 years, and the orbit's inclination relative to Earth is 48°.
GQ Lupi is a T Tauri star, with a variable apparent magnitude ranging from 11.3 at brightest and 14.3 at faintest. Its spectral type is K7Ve, with the 'e' indicating emission lines in the spectrum, which in classical T Tauri stars such as GQ Lupi results from a surrounding, extensive disk. The star has 1.03±0.05 times the mass of the Sun, 1.75+0.06
−0.07 times the Sun's radius, and an effective temperature of 4306±35 K. Its estimated age is 2.8+1.8
−1.1 million years, which is thought to be the same of GQ Lupi b.
GQ Lupi also likely has a more widely-separated stellar companion, named 2MASS J15491331-3539118 or GQ Lupi C. This star has a projected separation of from 2400 au from the primary, has roughly 0.15 times the mass of the Sun, 0.9 times the Sun's radius, and an effective temperature of 3200 K.
Emission by hydrogen in the near-infrared (Paschen-beta) was first detected in 2007 with the Very Large Telescope (VLT). This was interpreted as a sign of accretion of material from a disk. Additionally H-alpha emission was detected with Hubble.
As a very young object, GQ Lupi b is still embedded in its circumplanetary disk, composed by gas and dust, and accretes gas from it. The disk has a radius of 80±10 RJ and is inclined at 85.6±0.5° relative to Earth. There is evidence for a cavity within the disk, which has been suggested to be caused the accretion of dust by forming satellites. Thus, the disk of GQ Lupi b may be in its late stages where the formation of satellites is taking place and the inner parts were already cleared. The accretion rate of GQ Lupi b is estimated at 3.2×10−7 MJ per year.
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GQ Lupi b
GQ Lupi b, or GQ Lupi B is a substellar companion to the T Tauri star GQ Lupi. Classified as either an exoplanet or a brown dwarf, this object is still in the early stages of its formation, accreting gas from its circumplanetary disk. GQ Lupi b is orbiting at nearly 100 astronomical units from the star, with an estimated orbital period around a millennium. The object was discovered by R. Neuhäuser et al., through direct imaging and announced in April 2005, less than a month before the full confirmation of 2M1207b was announced. Along with 2M1207b, this was one of the first extrasolar planet candidates to be directly imaged.
GQ Lupi b was discovered in 2005 by a team led by R. Neuhäuser. By analysing data taken from the NACO adaptive optics aboard the Very Large Telescope, they discovered a faint companion to GQ Lupi A, and combining this with archival observations from the Subaru and Hubble Space Telescopes, they were able to confirm that the companion co-moves with the star and thus is gravitationally bound. At the time, this was considered to be the first direct imaging discovery of a planetary-mass companion orbiting a star. The image was made with the European Southern Observatory's VLT telescope at the Paranal Observatory, Chile on June 25, 2004. In 2006, the IAU's Working Group on Extrasolar Planets described GQ Lup b as a "possible planetary-mass companion to a young star".
GQ Lupi b is within the Lupus I molecular cloud, a star-forming region that is part of the Scorpius–Centaurus association. The cloud is located at a distance of roughly 460 ± 160 light-years (140 ± 50 parsecs). The GQ Lupi system is located at a distance of 501.7+2.2
−2.7 ly (153.82+0.67
−0.82 pc). As seen from Earth, it is within the constellation of Lupus.
GQ Lupi b orbits at a semi-major axis of 98 astronomical units from its host star, having a moderate orbital eccentricity of 0.35. This means that the farthest passage (apoastron) occurs at 132 au while the closest passage (periastron) occurs at 64 au. The orbital period is of roughly 920 years, and the orbit's inclination relative to Earth is 48°.
GQ Lupi is a T Tauri star, with a variable apparent magnitude ranging from 11.3 at brightest and 14.3 at faintest. Its spectral type is K7Ve, with the 'e' indicating emission lines in the spectrum, which in classical T Tauri stars such as GQ Lupi results from a surrounding, extensive disk. The star has 1.03±0.05 times the mass of the Sun, 1.75+0.06
−0.07 times the Sun's radius, and an effective temperature of 4306±35 K. Its estimated age is 2.8+1.8
−1.1 million years, which is thought to be the same of GQ Lupi b.
GQ Lupi also likely has a more widely-separated stellar companion, named 2MASS J15491331-3539118 or GQ Lupi C. This star has a projected separation of from 2400 au from the primary, has roughly 0.15 times the mass of the Sun, 0.9 times the Sun's radius, and an effective temperature of 3200 K.
Emission by hydrogen in the near-infrared (Paschen-beta) was first detected in 2007 with the Very Large Telescope (VLT). This was interpreted as a sign of accretion of material from a disk. Additionally H-alpha emission was detected with Hubble.
As a very young object, GQ Lupi b is still embedded in its circumplanetary disk, composed by gas and dust, and accretes gas from it. The disk has a radius of 80±10 RJ and is inclined at 85.6±0.5° relative to Earth. There is evidence for a cavity within the disk, which has been suggested to be caused the accretion of dust by forming satellites. Thus, the disk of GQ Lupi b may be in its late stages where the formation of satellites is taking place and the inner parts were already cleared. The accretion rate of GQ Lupi b is estimated at 3.2×10−7 MJ per year.
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