Astrophysics update 2 by John Mason

By John Mason

«Astrophysics Updates» is meant to serve the knowledge wishes astronomers and postgraduate scholars approximately parts of astronomy, astrophysics and cosmology which are wealthy and lively examine spheres. Observational equipment and the most recent result of astronomical learn are provided in addition to their theoretical foundations and interrelations. The contributed commissioned articles are written through top exponents in a layout that would attract expert astronomers and astrophysicists who're drawn to subject matters outdoors their very own particular parts of study. This choice of well timed stories can also allure the curiosity of complex beginner astronomers looking scientifically rigorous assurance.

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1989, The effect of gas and grain opacity on the cooling of brown dwarfs, Astrophys. I. , & Fan, X. 2002, Clouds and chemistry: Brown dwarf atmospheric properties from optical and infrared colors, Astrophys. R. 1999, Spectroscopic classification of late-M and L field dwarfs, Astron. S. 2003, The NIRSPEC brown dwarf spectroscopic survey. I. Low-resolution nearinfrared spectra, Astrophys. T. , & Yanagisawa, K. 2004, Spectral classification and effective temperatures of L and T dwarfs based on near-infrared spectra, Astrophys.

Indeed, one of the fundamental observational goals of neutron star astrophysics – some might say the “holy grail” – is to accurately place real neutron stars on such a plot of mass versus radius. Although the masses of some neutron stars, particularly pulsars in binary systems, have been very accurately determined, there is no accurate radius information for this sample (Thorsett & Chakrabarty 1999; Nice et al. 2004). The process of gravitational collapse which forms a neutron star leaves it incredibly hot.

The existence of such a superfluid is inferred from observations of sudden jumps (glitches) in the spin rates of pulsars (see Anderson & Itoh 1975; Link, Epstein & Lattimer 1999). As we proceed deeper, towards the core, the crustal lattice eventually dissolves, forming a stew of nucleons, electrons and muons. It is the core of the star, where most of the mass resides and where the densities are highest, that we would most like to probe, for a wide range of theoretical possibilities exist, and a narrowing down of these would tell us much about fundamental physics.

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