Astrophysics update 2 by John Mason

By John Mason

«Astrophysics Updates» is meant to serve the data wishes astronomers and postgraduate scholars approximately components of astronomy, astrophysics and cosmology which are wealthy and energetic study spheres. Observational equipment and the newest result of astronomical learn are offered in addition to their theoretical foundations and interrelations. The contributed commissioned articles are written via best exponents in a layout that might attract expert astronomers and astrophysicists who're attracted to subject matters open air their very own particular components of analysis. This choice of well timed reports can also allure the curiosity of complex beginner astronomers looking scientifically rigorous assurance.

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2004, Spitzer Infrared Spectrograph (IRS) Observations of M, L, and T dwarfs, Astrophys. J. Suppl. K. 2000, Molecular abundances in the atmosphere of the T dwarf Gl 229B, Astrophys. S. 2003, Non-equilibrium chemistry in the atmospheres of brown dwarfs. ASP Conf. Series IAU Symp. 211 on Brown Dwarfs (ed. N. 2001, Analysis of Keck HIRES spectra of early L-type dwarfs, Astrophys. D. 2002, Effective temperatures of late L dwarfs and the onset of methane signatures, Astrophys. , & Chanover, N. 2001, L-band photometry of L and T dwarfs, Astrophys.

This would have the effect of keeping stars with this quark matter phase in their cores, and older than about 10 million years, substantially warmer than “standard” cooling calculations would suggest. Thus, a detection of an old, warm neutron star could be an indication of the presence of quark matter in its interior. At present it is not known with any certainty at what densities these phases actually appear, and thus whether they actually occur in real neutron stars, however, further theoretical studies are warranted and might eventually yield a robust observational signature of quark matter.

However, several plausible destruction reactions are highly exothermic at 1000 K and should have activation energy factors close to zero FeH + OH → H2 O + Fe ∆H = −344 kJ mol−1 FeH + CH3 → CH4 + Fe ∆H = −288 kJ mol−1 FeH + H → H2 + Fe ∆H = −282 kJ mol−1 FeH + HS → H2 S + Fe ∆H = −228 kJ mol−1 FeH + FeH → H2 + 2Fe ∆H = −120 kJ mol−1 These reactions may proceed at rates close to the gas kinetic rate (10−10 – 10 cm3 s−1 ) and have chemical lifetimes much less than the vertical mixing times in the atmospheres of sub-stellar mass objects.

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