The Gliese 752 system consists of two M-type stars. The primary star is the magnitude9Gliese (GJ) 752 A. The secondary star is the dim magnitude17Gliese (GJ) 752 B, more commonly referred to as VB 10. This stellar pair form a binary star system separated by about 74 arc seconds (~434 AU).[8] This system is also known for its high proper motion of about 1 arc second a year. Component A has one known exoplanet.
The primary star, also known as Wolf 1055, is a type M2.5red dwarf with about half the size and mass as the Sun and considerably cooler at 3,534±51 K.[2] This star was first observed to be a high proper motion star by the German astronomer Max Wolf with his pioneering use of astrophotography. He added this star to his extensive catalog of such stars in 1919.[13] It is a variable star with the variable star catalog name V1428 Aquilae. It is a BY Draconis type variable star subject to flare events.[5][6]
In August 2018, a group of scientists using measurements taken from the CARMENES spectrograph, on the Calar Alto Observatory located in Spain, announced they had detected a planet orbiting the larger of the stars, HD 180617 (Gliese 752 A). The measurements indicated the presence of a planet with a minimum mass comparable to Neptune on an orbit partly located within the habitable zone.[9]
Gliese 752 was not known to be a binary star system until the discovery of a small dim secondary star by George Van Biesbroeck in 1944. This star is identified as VB 10inVan Biesbroeck's star catalog. This star is notable for its very low mass. At .08 solar masses, it is near the lower mass limit for a star. It is also quite small at 10% of the solar radius.[8]Atype M8Vred dwarf, the star is known for its very low luminosity (one of the least luminous stars yet observed)[14] with an absolute magnitude of nearly 19, due to its very cool surface temperature of only 2600K.[4] It is a variable star with the variable star catalog name V1298 Aquilae. This star is a UV Ceti type variable star also subject to flare events. It shares the large proper motion, along with the tendency to flare, with the primary star.[7]
In 2009, the discovery of the extrasolar planet, VB 10b, was announced in orbit around this star.[11] However a subsequent spectrographic survey failed to confirm the presence of any large planets in orbit around this star.[15]
In 1994, the Hubble Space Telescope observed a solar flare on Gliese 752 B. This suggests that the star has a strong magnetic field, which came as a surprise to astronomers. It had previously been assumed that low mass red dwarfs would have insignificant or nonexistent magnetic fields. These tiny dwarfs are supposed to lack the radiative zone just outside the star's core that creates the magnetic field-creating dynamos in more massive stars like our Sun. Nevertheless, the detection of solar flares indicates that as yet unknown process allows low mass stars to produce sufficient magnetic fields to power such outbursts, even if solely by convection, without a radiative core.[16]
^ abcdefghijklBurt, Jennifer; Feng, Fabo; Holden, Bradford; Mamajek, Eric E.; Huang, Chelsea X.; Rosenthal, Mickey M.; Wang, Songhu; Butler, R. Paul; Vogt, Steven S.; Laughlin, Gregory; Henry, Gregory W.; Teske, Johanna K.; Wang, Sharon X.; Crane, Jeffrey D.; Shectman, Steve A. (2021), "A Collage of Small Planets from the Lick–Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime", The Astronomical Journal, 161 (1): 10, arXiv:2011.08867, Bibcode:2021AJ....161...10B, doi:10.3847/1538-3881/abc2d0, S2CID227013469
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