By John W. Mason
"Astrophysics Updates" is meant to serve the data wishes astronomers and postgraduate scholars approximately parts of astronomy, astrophysics and cosmology which are wealthy and energetic learn spheres. Observational tools and the most recent result of astronomical study are provided in addition to their theoretical foundations and interrelations. The contributed commissioned articles are written via top exponents in a structure that would attract expert astronomers and astrophysicists who're attracted to issues outdoors their very own particular components of study. This number of well timed stories can also allure the curiosity of complicated beginner astronomers looking scientifically rigorous assurance.
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Additional info for Astrophysics Update 2 (Springer Praxis Books Astronomy and Planetary Sciences)
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.
Because of this, accreting neutron stars are arguably more promising sources for line searches. An encouraging recent result is the detection of absorption features in bursts from the LMXB 0748-676 with XMM-Newton (Cottam, Paerels & Mendez 2002). They found ≈ 10 eV equivalent width absorption features by co-adding 28 bursts seen with the Reﬂection Grating Spectrometers (RGS) spectrometers. 3 shows their RGS spectra and best model. 35 from the neutron star surface. Although extremely exciting, this remains so far a single detection, and the ubiquity of such features in X-ray bursts in general remains to be established with future observations.
A. 2002a, New CrH opacities for the study of L and brown dwarf atmospheres, Astrophys. , Hubeny, I. 2002b, Theoretical spectral models of T dwarfs at short wavelengths and their comparison with data, Astrophys. , & Volobuyev, M. 2003, Calculations of the far-wing line proﬁles of sodium and potassium in the atmospheres of substellar-mass objects, Astrophys. I. 2003, Beyond the T dwarfs: Theoretical spectra, colors, and detectability of the coolest brown dwarfs, Astrophys. , & Baraﬀe, I. H. 2000, Evolutionary models for very low-mass stars and brown dwarfs with dusty atmospheres, Astrophys.