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 learn spheres. Observational tools and the newest result of astronomical learn are provided in addition to their theoretical foundations and interrelations. The contributed commissioned articles are written by means of major exponents in a structure that might attract specialist astronomers and astrophysicists who're drawn to issues outdoor their very own particular components of analysis. This number of well timed stories can also allure the curiosity of complicated beginner astronomers looking scientifically rigorous insurance.

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3). 3–3 bar, the temperatures from the CH4 = CO boundary give 1180–1280 K. The lower bound in total pressure is that obtained for spectral type L6 above, and the upper bound comes from the positioning of the effective temperature of the T dwarf Gl 229B in Fig. 3. We plot the chemical temperature for T0 at 1230 K (at 2 bar). This chemical temperature coincides with the effective temperature at the L-T transition given by Burgasser et al. 2). However, only knowledge of methane and CO abundance ratios in late L and T dwarfs are good temperature diagnostics (Lodders & Fegley 2002) but this requires quantitative CO and methane abundance determinations which in turn require high-resolution model spectra for analyses.

Interestingly, the condensation curve of Cr metal and the equal abundance curve for Li = LiCl are positioned very close together (Figs. 3 bar), which is used as chemical temperature for L6. This temperature is only 50 K less than the effective temperature of 1570 K for L6 estimated by Vrba et al. (2004). 24 K. Lodders and B. Fegley, Jr. The chemical temperature at the L-T transition is related to the CH4 = CO boundary (Figs. 3). 3–3 bar, the temperatures from the CH4 = CO boundary give 1180–1280 K.

1 Hz, with perhaps a fourth feature at 28 Hz. In both flares these fast oscillations are only detected over a unique range of spin phase of each neutron star. This provides strong evidence that they are produced close to or, indeed, at the stellar surface, and are likely associated with a particular site on the star, perhaps the location of a crust fracture. If the observed frequencies are indeed those of global torsional oscillation modes, whose frequencies depend on the interior structure, then they could become a new, unique probe of neutron star structure.

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