Félix Llorente de AndrésInstituto Nacional de Técnica Aeroespacial | INTA · Villafranca European Space Astronomy Centre
Félix Llorente de Andrés
PhD
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22
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Introduction
Publications
Publications (22)
This work aims to investigate the behaviour of the lithium abundance in stars with and without detected planets. Our study is based on a sample of 1332 FGK main-sequence stars with measured lithium abundances, for 257 of which planets were detected. Our method reviews the sample statistics and is addressed specifically to the influence of tides and...
The nature of the few known solar-mass stars simultaneously containing debris disks and planets remains an open question. A number of works have shown that this property appears to be independent of planetary masses as well as of stellar age, but possible correlations with stellar kinematics and metallicity have not been investigated. In this paper...
The nature of the few known solar-mass stars simultaneously containing debris disks and planets remains an open question. A number of works have shown that this property appears to be independent of planetary masses as well as of stellar age, but possible correlations with stellar kinematics and metallicity have not been investigated. In this paper...
We developed a mathematical model to derive time scales and the presence of BS stars. The model is based on the variation of mass through a circle into the cluster defined by a radius, and at a time; this mass cross is translated into a differential equation that it can be integrated for a given radius (r) and a determined time (t). From this equat...
Context. The lithium abundance, A (Li), in stellar atmospheres suffers from various enhancement and depletion processes during the star’s lifetime. While several studies have demonstrated that these processes are linked to the physics of stellar formation and evolution, the role that Galactic-scale events play in the galactic A (Li) evolution is no...
The lithium abundance, A(Li), in stellar atmospheres suffers from various enhancement and depletion processes during the star's lifetime. While several studies have demonstrated that these processes are linked to the physics of stellar formation and evolution, the role that Galactic-scale events play in the galactic A(Li) evolution is not yet well...
We investigate two topics regarding solar mass FGK-type stars, the lithium-rotation connection (LRC), and the existence of the ‘lithium desert’. We determine the minimum critical rotation velocity ( v sin i ), related with the LRC separating slow from rapid stellar rotators, to be 5 km s ⁻¹ . This value also splits different stellar properties. For...
We investigate two topics regarding solar mass FGK-type stars, the lithium rotation connection (LRC) and the existence of the "lithium desert". We determine the minimum critical rotation velocity ($v \sin i$) related with the LRC separating slow from rapid stellar rotators, as being 5 km s$^{-1}$. This value also split different stellar properties....
Dwarf stars with debris discs and planets appear to be excellent laboratories to study the core accretion theory of planets formation. These systems are however, insufficiently studied. In this paper we present the main metallicity and lithium abundance properties of these stars together with stars with only debris discs and stars with only planets...
Dwarf stars with debris discs and planets appear to be excellent laboratories to study the core accretion theory of planets formation. These systems are however, insufficiently studied. In this paper we present the main metallicity and lithium abundance properties of these stars together with stars with only debris discs and stars with only planets...
It is suggested that a group of a southern T-Tauri stars presented by V
4046 Sgr (HDE 319139), Co-2711363, AS 218, and TW Hya, located
relatively far from any known dark or molecular clouds, were formed in
very small clouds leaving almost no residuals, instead of having escaped
from a cloud as suggested in the past of a similar isolated T-Tauri typ...
Software for correcting and processing echelle spectrograms is
developed. Without knowing them a priori, the geometric deformations of
these spectrograms are obtained. The algorithms can be implemented in a
minicomputer with a capability of 128 Kbytes. The time for reducing one
spectrum is less than 6 min. The accuracy of the method in wavelength
c...
The profiles of the ultraviolet C IV resonance lines of 6 O-type stars
in IC 1805 observed by the IUE satellite are examined. The mass loss
rates are determined by means of the fitting of theoretical line
profiles on the observed lines. M varies as L to the 1.33 power, in
qualitative agreement with the most recent parametrization of the
dependence...
Ultraviolet intrinsic colors of early type stars observed by the S2/68
Sky Survey Telescope in the TD-1A satellite are presented. These
ultraviolet intrinsic colors are computed in the spectral region from
1380 to 2540 A in wavelength intervals of 20 A and in the photometric
band of about 330 A width centered at 2740 A. The accuracy of the
intrinsi...
It is noted that rapid rotation introduces an intrinsic reddening, which is significant for the rapidly rotating Be stars, in particular the B0e. In fact, a correlation is found between E(B-V) and vsini for B0 and B4 stars. Neglecting this effect produces an overestimate of interstellar reddening which in turn yields an overcorrection of ultraviole...
From a sample of about 100 reddened early type stars, a mean
interstellar extinction law in the wavelength range from 2740 to 1380
Å has been derived by means of a grid of ultraviolet intrinsic
colours. The ultraviolet spectra were obtained with the Sky Survey
telescope (S2/68) in the TD-l satellite. It is found that the mean
extinction curve in te...
From a large sample of reddened stars we computed the individual extinction curves which agree with that calculated by Nandy et al. (1976), except for four stars which show that the extinction at the 2200 Å feature is greater than that deduced for the rest of stars. These four stars belong to the Cassiopeia-Taurus association.
For early B main-sequence and giant stars the observed near-UV blocking factors are larger than those predicted by blanketed model atmospheres with a microturbulence of 2 km/sec. Better agreement would be reached if a microturbulence of 4 to 5 km/sec were adopted. Evidence was found that the line opacities due to doubly ionized metals are unsuffici...
The ultraviolet C IV resonance lines of seven O-type stars in IC 1805
were observed with the IUE satellite in the low dispersion mode in the
1150-1950 A and 1900-3200 A wavelength ranges. The spectra showed very
large and deep P Cygni profiles of the C IV resonance doublet at 1548.20
A and 1550.77 A, and P Cygni characteristics increased with bolom...