infinite
发表于 2025-3-25 07:20:24
Activity and Kinematics of M and L Dwarfst. The frequency and strength of chromospheric activity disappears rapidly as a function of temperature over spectral types M8-L4. There is evidence that young late-M and L dwarfs have weaker activity than older ones (the opposite of the traditional stellar age-activity relation). The kinematics of
fender
发表于 2025-3-25 08:43:59
Infrared Spectroscopy of Brown Dwarfs: the Onset of CH4 Absorption in L Dwarfs and the L/T Transitio Survey contain absorption bands of both methane and carbon monoxide and bridge the gap between late L and previously observed T dwarfs. These dwarfs form a clear spectral sequence, with CH. absorption increasing as the CO absorption decreases. Water vapor band strengths increase in parallel with th
高贵领导
发表于 2025-3-25 12:18:51
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Eviction
发表于 2025-3-25 18:44:43
Low-Mass Stellar and Brown Dwarf Binary Systems range of the HR diagram. Most notably, the overwhelming majority of measurements of mass, the fundamental stellar parameter, rest on observations of astrometric or spectroscopic binaries. For main sequence stars, those individual measurements can be combined to define a mass-luminosity relation whi
松紧带
发表于 2025-3-25 20:24:25
Low-Luminosity Companions to Nearby Stars: Status of the 2MASS Data Searches, we estimate masses for these discoveries and compare them to four other L and T dwarf companions from the literature. Temperatures range from ~2000 to ~750 K, ages range from ~0.2 to ~3 Gyr, and masses range from ~0.035 to ~0.075 MO.
羊齿
发表于 2025-3-26 03:14:50
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Formidable
发表于 2025-3-26 04:29:14
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贪心
发表于 2025-3-26 08:33:45
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率直
发表于 2025-3-26 14:56:46
Conference proceedings 2001. Yet it took until 1850 to realise that fainter stars were not necessarily further away, nor the brighter ones closer. In fact within the magnitude range observable to the naked eye it is probable that the brighter star is in fact further away. Even today the measurement of stellar distances is rel
Trabeculoplasty
发表于 2025-3-26 20:00:46
Formation of the Optical Spectra of L Dwarfs spectral classes are analyzed. The computed spectral energy distributions (SED’s) of L dwarfs are compared to the observed spectra. Perspectives of Lithium and Deuterium tests to assess the new populations of the Galaxy have been considered.