Based on the lithium test, it is likely that roughly two-thirds of all L dwarfs are true stars. If it does not have lithium, then the object is likely a true star. Stars tend to burn away all of its lithium very quickly while brown dwarfs do not so if an L-type fusor has lithium in its spectrum, then it is likely that the object is a brown dwarf. A test that can be used to distinguish between L-type stars and L-type brown dwarfs is the lithium test. CrH and FeH) and alkali metal bands (e.g. TiO and VO)-a defining feature of Class M stars, and the presence of strong metallic hydride bands (e.g. The spectra of Class L stars are characterized by weak or nonexistent metallic oxide bands (e.g. One of the least energetic known main sequence stars is a star of spectral type L2.5 V called 2MASS J0523−1403-a star with a mass comparable to the minimum possible mass for a star. Properties of L-type main sequence stars Ĭlass L main sequence stars and less massive Class M stars that will evolve into Class L stars are the least massive and coolest possible stars capable of hydrogen fusion. 2 Evolution of L-type main sequence stars.1 Properties of L-type main sequence stars.Such supergiants likely cannot form from typical stellar evolution and have to be created via collisions of stars. V838 Monocerotis is a known example of an L-type supergiant candidate. While most Class L stars are either very massive brown dwarfs or less massive main sequence stars, it may be possible for atypically cool supergiant stars to be examples of Class L stars. This combined with the low temperatures, leave Class L stars extremely poor candidates for life. This close distance would leave the planet tidally locked to the star. They appear to be a dim orange to orange-red with their spectrum peaking in the infrared.Ĭlass L stars often begin their life with emissions in the Class M spectrum with a temperature of over 3,000 K but cool off and become dimmer over time.Ĭlass L stars have a habitable zone in between 0.007 and 0.04 AU, or between 1,050,000 to 6,700,000 km, which is 10 - 54 times as close as Mercury's orbit to the Sun. More massive Class L stars are at the limits of smallest stars capable of fusing hydrogen, whereas less massive ones fuse deuterium and lithium instead. They are generally 65 - 90 times as massive as Jupiter and their temperature is generally 1,300 - 2,400 K. A Class L star is a stellar class that includes early brown dwarfs and ultracool low mass stars.
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