MOA-2010-BLG-477L

MOA-2010-BLG-477L is a K-type star with about 0.67 times the mass of the Sun,[1] in the main-sequence phase of its stellar evolution.[1] Overall, very little is known about this star, with very poor constrains on its projected characteristics due to One extrasolar planet, with a mass greater than that of Jupiter, has been discovered orbiting the star at a distance of roughly 2 AU.[2] The planet was detected by means of microlensing,[1] where gravitational lensing as the planet and its host star pass in front of a background star causes a temporary flare in the amount of light observed, allowing the planet's existence to be known.[1]

MOA-2010-BLG-477L
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittiarus
Right ascension  18h 06m 7.44s[1]
Declination −31° 24′ 16.12″[1]
Characteristics
Spectral type KV[1]
Variable type unknown
Astrometry
Distance7500 ± 2000[2] ly
(2300 ± 600[2] pc)
Details
Mass0.67+0.33
−0.13[2] M☉
Database references
SIMBADdata

Planetary system

The history of the detection of the planet, MOA-2010-BLG-477 L b, dates back to the year 2010. In that year, a microlensing alert event occurred, before the planet was confirmed conclusively, and was detected independently by the MOA and OGLE collaborations.[1] Following the original microlensing event, astronomers predicted another microlensing peak, which was observed by numerous groups using a wide array of telescopes.[1] One of these telescopes was located in Antarctica, and made the first microlensing detections from that continent; however, the data collected there were too crude to be included in the analysis which eventually confirmed the planet.[1]

MOA-2010-BLG-477 L b is the only planet which has been detected orbiting MOA-2010-BLG-477 L. Little is known about this planet, with the only characteristics known about this system are the mass of the planet and its projected separation from its host star.[2]

The MOA-2010-BLG-477L planetary system[2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.5−0.3+1.8 MJ 2−1+3 — — — —
gollark: Probably would be worth asking on their discord server beforehand about things.
gollark: If mgollark² is to occur, I would probably construct them by using Google Colab to obtain fast TPUs for training, then somehow having you download the 12GB of bee neuron data to something connected to this "coral TPU".
gollark: Not practical. For mgollark I just harvested some free Google computing power.
gollark: https://github.com/EleutherAI/gpt-neo seems to mention TPU support, although it wants high-powered "cloud" ones for training, no idea what it needs for inferencing.
gollark: Wait, you have a TPU, right citrons?

References
  1. Bachelet, E.; Shin, I.-G.; Han, C.; Fouqué, P.; Gould, A.; Menzies, J. W.; Beaulieu, J.-P.; Bennett, D. P.; et al. (2012). "MOA-2010-BLG-477Lb: Constraining the mass of a microlensing planet from microlensing parallax, orbital motion and detection of blended light". arXiv:1205.6323. Bibcode:2012ApJ...754...73B. doi:10.1088/0004-637X/754/1/73. Cite journal requires |journal= (help)
  2. Schneider, Jean (2 June 2012). "Notes for Star MOA-2010-BLG-477L". The Extrasolar Planets Encyclopaedia.
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