Galaxy Assembly through Mergers
... to make me smile and a word to comfort me. Thank you for being my safe haven. My friends have been the backbone of my life, especially in the last few years. Ana and Pedro, my partners in crime, thank you for bearing with me in the most turbulent of times, never leaving my side. I thank you for the ...
... to make me smile and a word to comfort me. Thank you for being my safe haven. My friends have been the backbone of my life, especially in the last few years. Ana and Pedro, my partners in crime, thank you for bearing with me in the most turbulent of times, never leaving my side. I thank you for the ...
kdtalk_jun2005 - The HST Treasury Program on Eta Carinae
... Certainly L > 3 million L sun , and probably ...
... Certainly L > 3 million L sun , and probably ...
Photometric Variability and Rotation in Magnetic White Dwarfs
... initiating me into the mysteries of observing and the techniques of operating the INT in La Palma and the 1.0m telescope in South Africa. There are many memories, especially from observing trips, that will stay with me forever. I am indebted to numerous people around the world who have been observin ...
... initiating me into the mysteries of observing and the techniques of operating the INT in La Palma and the 1.0m telescope in South Africa. There are many memories, especially from observing trips, that will stay with me forever. I am indebted to numerous people around the world who have been observin ...
The Day We Found the Universe
... happily changed to civil reckoning for determining the start of a day. No longer would the astronomical day begin at high noon, a tradition launched in the days of Ptolemy that often led to great bookkeeping confusion. Instead, it now began at midnight, just as it did for everyone else. “It will pro ...
... happily changed to civil reckoning for determining the start of a day. No longer would the astronomical day begin at high noon, a tradition launched in the days of Ptolemy that often led to great bookkeeping confusion. Instead, it now began at midnight, just as it did for everyone else. “It will pro ...
Deformations of Accreting Neutron Star Crusts and Gravitational
... spin equilibrium (where the spin frequency matches the Keplerian frequency at the magnetosphere) at nearly identical spin frequencies. This requires that the neutron star’s dipolar magnetic field strength correlates very well with Ṁ (White & Zhang 1997; Miller, Lamb, & Psaltis 1998). In an alternat ...
... spin equilibrium (where the spin frequency matches the Keplerian frequency at the magnetosphere) at nearly identical spin frequencies. This requires that the neutron star’s dipolar magnetic field strength correlates very well with Ṁ (White & Zhang 1997; Miller, Lamb, & Psaltis 1998). In an alternat ...
The 3-D shaping of NGC 6741: a massive, fast
... valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, ionic and chemical abundances) integrated over the whole sli ...
... valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, ionic and chemical abundances) integrated over the whole sli ...
Post-Common-Envelope Binaries from the Sloan Digital Sky Survey
... I deeply thank Dr. Boris Gänsicke for his excellent guidance through my PhD, for his help and suggestions, and most importantly for making it possible for me to develop my qualities as a researcher. I am also deeply thankful for his trust in me in this and other projects. Without him this thesis wo ...
... I deeply thank Dr. Boris Gänsicke for his excellent guidance through my PhD, for his help and suggestions, and most importantly for making it possible for me to develop my qualities as a researcher. I am also deeply thankful for his trust in me in this and other projects. Without him this thesis wo ...
arXiv:astro-ph/0702414v1 15 Feb 2007
... be less affected by dust than the continuum radiation in a twophase interstellar medium. Moreover, a large-scale outflow of neutral gas can decrease the number of Lyα resonance scattering (Kunth et al. 1998), if the neutral gas is velocity-shifted with respect to the ionised gas. To conclude, interp ...
... be less affected by dust than the continuum radiation in a twophase interstellar medium. Moreover, a large-scale outflow of neutral gas can decrease the number of Lyα resonance scattering (Kunth et al. 1998), if the neutral gas is velocity-shifted with respect to the ionised gas. To conclude, interp ...
Europium, Samarium, and Neodymium Isotopic Fractions in Metal
... where the lines of interest are concentrated, (2) absorption lines of all species will exhibit greater line depth in giants than in dwarfs because of the decrease in the continuous opacity with decreasing electron pressure in giants, and (3) at a given metallicity, molecular formation will be less i ...
... where the lines of interest are concentrated, (2) absorption lines of all species will exhibit greater line depth in giants than in dwarfs because of the decrease in the continuous opacity with decreasing electron pressure in giants, and (3) at a given metallicity, molecular formation will be less i ...
arXiv:astro-ph/0703091v1 5 Mar 2007
... survey specifically designed to identify and supply initial high-resolution abundance analyses of up to nine elements in new n-capture-rich candidates. Over 40 new r-process-rich stars were reported in that paper. More such stars will undoubtedly be discovered as the high-resolution survey work cont ...
... survey specifically designed to identify and supply initial high-resolution abundance analyses of up to nine elements in new n-capture-rich candidates. Over 40 new r-process-rich stars were reported in that paper. More such stars will undoubtedly be discovered as the high-resolution survey work cont ...
Cool Subdwarf Investigations (CSI) I: New Thoughts for the Spectral
... three categories: regular dwarfs, subdwarfs, and extreme subdwarfs. Numerical subclasses were then assigned using two independent linear fits for subdwarfs and extreme subdwarfs. ...
... three categories: regular dwarfs, subdwarfs, and extreme subdwarfs. Numerical subclasses were then assigned using two independent linear fits for subdwarfs and extreme subdwarfs. ...
The Early Evolution of Solids in Protoplanetary Disks
... and going up to the gas-accretion phase leading to the build up of rocky planets and gas giants. The first stages of this process are characterized by collisional growth of tiny subµm sized grains, as those found in the interstellar medium. Observations in the millimeter can directly probe the exist ...
... and going up to the gas-accretion phase leading to the build up of rocky planets and gas giants. The first stages of this process are characterized by collisional growth of tiny subµm sized grains, as those found in the interstellar medium. Observations in the millimeter can directly probe the exist ...
H-alpha Imaging of Early-type (Sa
... in most early-type spirals is less than 1039 ergs−1. However, we also find that a significant fraction (15 − 20%) of early-type spirals do have at least one H II region in the disk with LHα ≥ 1039 ergs−1. The latter result is not necessarily in contrast to Caldwell’s study for two reasons. First, Ca ...
... in most early-type spirals is less than 1039 ergs−1. However, we also find that a significant fraction (15 − 20%) of early-type spirals do have at least one H II region in the disk with LHα ≥ 1039 ergs−1. The latter result is not necessarily in contrast to Caldwell’s study for two reasons. First, Ca ...
The 3-D shaping of NGC 6741: A massive, fast
... Abstract. We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position an ...
... Abstract. We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position an ...
Physics of Neutron Star Crusts - Institut d`Astronomie et d
... to the description of the wealth of neutrino emission processes associated with the crust. We limit there to the basic mechanisms, which according to existing calculations are the most important ones at subsequent stages of neutron star cooling. Confrontation of theory with observations is presented ...
... to the description of the wealth of neutrino emission processes associated with the crust. We limit there to the basic mechanisms, which according to existing calculations are the most important ones at subsequent stages of neutron star cooling. Confrontation of theory with observations is presented ...
Physics of Neutron Star Crusts
... to the basic mechanisms, which, according to existing calculations, are the most important ones at subsequent stages of neutron-star cooling. The confrontation of theory with observations is presented in Section 12. Neutron stars are born very hot, and we briefly describe in Section 12.1 the present ...
... to the basic mechanisms, which, according to existing calculations, are the most important ones at subsequent stages of neutron-star cooling. The confrontation of theory with observations is presented in Section 12. Neutron stars are born very hot, and we briefly describe in Section 12.1 the present ...
Mid-infrared Properties of Seyfert Galaxies: the IRAS 12um Sample
... In starbursts the 11.2μm PAH flux correlates with the IRAS 12μm continuum In Seyferts there is an extra contribution due to the AGN warm dust emission Can we quantify this in a statistical manner? SHAO - Oct 2010 ...
... In starbursts the 11.2μm PAH flux correlates with the IRAS 12μm continuum In Seyferts there is an extra contribution due to the AGN warm dust emission Can we quantify this in a statistical manner? SHAO - Oct 2010 ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.