Titlebook: Ultracool Dwarfs; New Spectral Types L Hugh R. A. Jones,Iain A. Steele Conference proceedings 2001 Springer-Verlag Berlin Heidelberg 2001 B

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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

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

高貴領(lǐng)導(dǎo)

Eviction

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

松緊帶

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.

羊齒

Formidable

貪心

率直

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

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.