We contribute to the subject of the physical interpretation of exact solutions by characterizing them through a systematic study in terms of unambiguous physical concepts coming from systems in linearized gravity. We use the physical meaning of the leading order behavior of the Weyl spinor components $Psi_0^0$, $Psi_1^0$ and $Psi_2^0$ and of the
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Characterizing exact solutions from asymptotic physical conceptsPerez, Alejandro et al.122000
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Chemical abundances from the continuum
The calculation of solar absolute fluxes in the near-UV is revisited, discussing in some detail recent updates in theoretical calculations of bound free opacity from metals. Modest changes in the abundances of elements such as Mg and iron-peak elements have a significant impact on atmospheric structure, and therefore self-consistent calculations
Allende Prieto, C.Advertised on:
122008 -
Chemical Abundances of Volatiles and Refractories in Solar Analogs with and without Planets: No Relation with Terrestial Planets
We present the abundances of volatile and refractory elements in the atmospheres of 95 solar analogs, 24 planet hosts and 71 "single" stars, to investigate its possible connection with terrestial planets, using very high-quality HARPS and UVES spectra. The whole sample of stars with and without planets show almost the same mean abundance pattern
González Hernández, J. I. et al.Advertised on:
122011 -
Chemical Clues on the Formation of Planetary Systems: C/O Versus Mg/Si for HARPS GTO Sample
Theoretical studies suggest that C/O and Mg/Si are the most important elemental ratios in determining the mineralogy of terrestrial planets. The C/O ratio controls the distribution of Si among carbide and oxide species, while Mg/Si gives information about the silicate mineralogy. We present a detailed and uniform study of C, O, Mg, and Si
Delgado-Mena, E. et al.Advertised on:
122010 -
Chemical Properties of Stars with Giant Planets
Not Available
Santos, N. C. et al.Advertised on:
122006 -
Chemical Signature of Gas-rich disc-disc Mergers at high Redshift
We performed numerical simulations of mergers between gas-rich disc galaxies, which result in the formation of late-type galaxies. Stars formed during the merger end up in a thick disc that is partially supported by velocity dispersion and has high [α/Fe] ratios at all metallicities. Stars formed later end up in a thin, rotationally supported disc
Martel, Hugo et al.Advertised on:
122011