Habitable Zones (HZs) of solar-type stars

P. MIQUELARENA; C. SAFFE; M. FLORES

La Serena

Congreso; The Second Binational Meeting AAA-SOCHIAS; 2018

Sociedad Chilena de Astronomía, Asociación Argentina de Astronomía

Since the discovery of the rst extrasolar planet around the star 51 Peg by Mayor I and Queloz (1995), many work groups have devoted themselves to nding these low mass companions around nearby stars. In particular, they deserve special attention to the so-called "terrestrial planets", which are rocky objects that are found within the so-called "Habitable Zone" (HZ) of the star. It is dened as a region around the star within which planets could keep liquid water on its surface (for example, Kasting et al., 1993), considered one of themost important conditions for its habitability. In the case of the Solar System, the HZ was found between 0.99 AU and 1.70 AU (Kopparapu et al. 2013), the Earth being then at a distance of 1.00 AU from the Sun, very close to the lower edge. The detailed calculation of the HZ is a complex process that includes the model of  at atmospheres through the so-called General Circulation Model (GCM). The internal and external radios of the HZ depend on variables such as the albedo and the chemical technology adopted for the planet (for example, Kasting et al., 1993, Kopparapu et al., 2013). Currently there are detailed calculations and HZ grids for main sequence stars (Kopparapu et al., 2013, 2014, Chandler et al., 2016). These grids depend primarily on the fundamental parameters of the corresponding stars, being important in the calculation of them. In this paper we present the calculation of the HZ regions of a sample of 100 stars of spectral types FGK. To do this, divide the work into three parts. First, the observation of a sequence of FGK stars of the main sequence in the CASLEO (Complejo Astronomico El Leoncito) is carried out. The spectra claim to be reduced and prepared for further analysis. Second, based on the observations made, the fundamental parameters of the stars will be calculated homogeneously using the FUNDPAR program (Sae 2011, Sae et al., 2015). Finally, the parameters for the estimation of the HZ of each of the stars follow the suggested guidelines for the calculation of Rint and Rout in stars of main sequence (Kopparapu et al. 2013, 2014, Muller I & Haghighipour 2014).