ULAS1350 has been classified as a subdwarf of type L and is the fifth of its class to be discovered to date and the first one confirmed by the GTC. ❋ Unknown (2009)
“Hera is the third planet of 492 Lyncis, a class G-2 subdwarf star approximately twelve hundred and seventeen light-years from Earth,” Data said. ❋ W.R. Thompson (1996)
The star in question, KIC 05807616, has a rather interesting description: "a seemingly isolated pulsating hot B subdwarf." ❋ John Timmer (2011)
We propose a SNAP-style program of single orbit FGS TRANS mode observations of very massive stars in the cluster NGC 3603, luminous blue variables, nearby low mass main sequence stars, cool subdwarf stars, and white dwarfs. ❋ Unknown (2010)
It belongs to a class of stars known as helium-rich hot subdwarf stars, researchers said. ❋ Unknown (2010)
The team also suggests that the star is shrinking from being a bright cool giant to a faint hot subdwarf. ❋ Unknown (2010)
X-ray bright systems, (5) find binaries among ancient and nearby subdwarf stars, and (6) help calibrate the white dwarf mass - radius relation. ❋ Unknown (2009)
SNAP-style program of single orbit FGS TRANS mode observations of very massive stars in the cluster NGC 3603, luminous blue variables, nearby low mass main sequence stars, cool subdwarf stars, and white dwarfs. ❋ Unknown (2009)
The X-ray pulsator RX J0648. 0-4418 and the subdwarf star HD49798 form a binary system with unique properties. ❋ Unknown (2009)
The photometric telescope would measure the brightness of some galaxy that the 2.5-meter telescope would also look at, compare the star not to Vega which was too bright even for the photometric telescope but to an F subdwarf star named BD+17, which had already been calibrated to Vega, then measure everything else that affected the galaxy’s brightness—atmosphere, dust, pollen, humidity—then adjust the galaxy’s brightness accordingly. ❋ Ann Finkbeiner (2010)
These observations will help us to (1) identify systems suitable for follow up studies for mass determination, (2) study the role of binaries in stellar birth and in advanced evolutionary states, (3) explore the fundamental properties of stars near the main sequence-brown dwarf boundary, (4) understand the role of binaries for X-ray bright systems, (5) find binaries among ancient and nearby subdwarf stars, and (6) help calibrate the white dwarf mass - radius relation. ❋ Unknown (2010)
