The Early Evolution of Solids in Protoplanetary Disks
... In this Thesis I obtained and analyzed new data in the millimetre for a sample of more than 50 young disks in three nearby star forming regions (Taurus, Ophiuchus, Orion); for all these sources I derived some of the main properties of dust particles, such as grain size and total mass. The results of ...
... In this Thesis I obtained and analyzed new data in the millimetre for a sample of more than 50 young disks in three nearby star forming regions (Taurus, Ophiuchus, Orion); for all these sources I derived some of the main properties of dust particles, such as grain size and total mass. The results of ...
Document
... class of variables because it was: – Among one of the brightest members of the new class – The best studied of the sample – Showed a good range of the absorption/emission features used to characterize the set of stars ...
... class of variables because it was: – Among one of the brightest members of the new class – The best studied of the sample – Showed a good range of the absorption/emission features used to characterize the set of stars ...
The VIMOS Ultra-Deep Survey (VUDS): Fast Increase in the Fraction
... Deharveng et al. 2008; Hayes et al. 2014). As a result of their nature, Lyα photons are found to be scattered at much larger scales than UV photons (Steidel et al. 2011; Momose et al. 2014). Predicting the escape fraction of the Lyα photons as a function of the galaxy properties involves including a ...
... Deharveng et al. 2008; Hayes et al. 2014). As a result of their nature, Lyα photons are found to be scattered at much larger scales than UV photons (Steidel et al. 2011; Momose et al. 2014). Predicting the escape fraction of the Lyα photons as a function of the galaxy properties involves including a ...
On the characterisation of the Galactic warp in the Gaia era
... all of your support and patience, aspiring guidance and immense knowledge. You always made time to help and advise me. I have been a pleasure for me to work with you. Also, I really appreciate you being so sensitive and supportive towards women’s right. Thank you Luis for being such an incredible te ...
... all of your support and patience, aspiring guidance and immense knowledge. You always made time to help and advise me. I have been a pleasure for me to work with you. Also, I really appreciate you being so sensitive and supportive towards women’s right. Thank you Luis for being such an incredible te ...
Revising the census of low luminosity AGN
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
FY96
... greater than 10 km/s in observations separated by 11 months. Including the efficiency for discovering binaries with different periods and orbital parameters, Cote and Fischer's result yields a binary fraction of 15% in M4. In a companion study, Cote, Carlton Pryor (Rutgers U.), Robert McClure, J.M. ...
... greater than 10 km/s in observations separated by 11 months. Including the efficiency for discovering binaries with different periods and orbital parameters, Cote and Fischer's result yields a binary fraction of 15% in M4. In a companion study, Cote, Carlton Pryor (Rutgers U.), Robert McClure, J.M. ...
Astronomy Astrophysics
... disk field is subsequently divided into 152 tiles, while the bulge field contains 196 tiles (Fig. 1). The data reduction was carried out in the canonical manner associated with infrared imaging, and details of the procedure are described by Irwin et al. (2004). In Borissova et al. (2011) we searched ...
... disk field is subsequently divided into 152 tiles, while the bulge field contains 196 tiles (Fig. 1). The data reduction was carried out in the canonical manner associated with infrared imaging, and details of the procedure are described by Irwin et al. (2004). In Borissova et al. (2011) we searched ...
Communications in Asteroseismology
... the first results from space asteroseismology are available? Isn’t it odd to celebrate the 65th birthday of a renowned asteroseismologist who is far from retirement at this point? The answer to the first question is easy: at the outset of this meeting, MOST was already in space and COROT was soon to b ...
... the first results from space asteroseismology are available? Isn’t it odd to celebrate the 65th birthday of a renowned asteroseismologist who is far from retirement at this point? The answer to the first question is easy: at the outset of this meeting, MOST was already in space and COROT was soon to b ...
SkyWatcher2017.5 1.3 Mb - Boise Astronomical Society
... 5/26 The Moon is at perigee, subtending 33' 27'' from a distance of 357,210 kilometers (221,958 miles), at 1:21; a double Galilean satellite shadow transit begins at 5:47; Mercury is at its greatest latitude south of the ecliptic plane (-7.0 degrees) at 20:00 5/27 Mars is 5.3 degrees north of the Mo ...
... 5/26 The Moon is at perigee, subtending 33' 27'' from a distance of 357,210 kilometers (221,958 miles), at 1:21; a double Galilean satellite shadow transit begins at 5:47; Mercury is at its greatest latitude south of the ecliptic plane (-7.0 degrees) at 20:00 5/27 Mars is 5.3 degrees north of the Mo ...
Understanding Variable Stars - Central Florida Astronomical Society
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
H i AND CO IN BLUE COMPACT DWARF GALAXIES: HARO 2 AND
... 2003), blowout of material into the halo occurs that will remove the products of nucleosynthesis in stars more massive than 8 M and disperse those across a larger volume. Numerical simulations have suggested that in extreme cases blow-away can occur, which removes these products from the galaxy pro ...
... 2003), blowout of material into the halo occurs that will remove the products of nucleosynthesis in stars more massive than 8 M and disperse those across a larger volume. Numerical simulations have suggested that in extreme cases blow-away can occur, which removes these products from the galaxy pro ...
Differential rotation in Sun-like stars from surface variability and
... The rotation of a star on the PMS sets the stage for all further evolution of its rotation rate on the MS and beyond. The exact nature however, of the AM evolution during these very early phases of stellar evolution is still poorly understood. This is in part because the only available indicator of ...
... The rotation of a star on the PMS sets the stage for all further evolution of its rotation rate on the MS and beyond. The exact nature however, of the AM evolution during these very early phases of stellar evolution is still poorly understood. This is in part because the only available indicator of ...
W.M. Keck Observatory Annual Report 2009
... II telescope to measure the spectrum of light emitted by each object to determine their composition and distance. The Keck spectra showed that the light from the supernovae traveled nearly 11 billion light years to reach Earth. Prior to this discovery, the astronomical literature showed that the mos ...
... II telescope to measure the spectrum of light emitted by each object to determine their composition and distance. The Keck spectra showed that the light from the supernovae traveled nearly 11 billion light years to reach Earth. Prior to this discovery, the astronomical literature showed that the mos ...
365 days of SKYWATCHING
... it’s possible to watch as the Earth overtakes a planet, much like running past an object on a racetrack. As we approach it, it will seem to slow down, stand still, and then move backwards as we go by. Once we have passed, it will then appear to resume forward motion. Since Mercury and Venus are on t ...
... it’s possible to watch as the Earth overtakes a planet, much like running past an object on a racetrack. As we approach it, it will seem to slow down, stand still, and then move backwards as we go by. Once we have passed, it will then appear to resume forward motion. Since Mercury and Venus are on t ...
my dissertation (PhD. Thesis) - Argelander
... Moreover they are the sites of the formation of stars such as our Sun. Therefore knowledge about their morphology and evolutionary history is of utmost importance for the understanding of the structure formation process in the universe and hence the process which in the end leads to the birth of sta ...
... Moreover they are the sites of the formation of stars such as our Sun. Therefore knowledge about their morphology and evolutionary history is of utmost importance for the understanding of the structure formation process in the universe and hence the process which in the end leads to the birth of sta ...
the PDF - Montana State University
... conclude that the physical conditions conducive to a quasi-periodic magnetic activity cycle like the Sun’s are rare in stars of approximately the solar mass, and that the proper conditions may be restricted to a relatively narrow range of rotation rates. ...
... conclude that the physical conditions conducive to a quasi-periodic magnetic activity cycle like the Sun’s are rare in stars of approximately the solar mass, and that the proper conditions may be restricted to a relatively narrow range of rotation rates. ...
X-ray astronomy of stellar coronae (Review)
... 2. The study of stellar coronae The study of stellar coronae, of course, starts with the Sun. This provides a rather important advantage for stellar astronomers: that of having a nearby, bright standard example available at high spatial and spectral resolution. What, then, should we expect from the ...
... 2. The study of stellar coronae The study of stellar coronae, of course, starts with the Sun. This provides a rather important advantage for stellar astronomers: that of having a nearby, bright standard example available at high spatial and spectral resolution. What, then, should we expect from the ...
Report from the Subaru Telescope for External
... Subaru Telescope (observatory) is a branch of the National Astronomical Observatory of Japan operating the 8.2-meter (effective aperture) optical-infrared telescope “Subaru” located at the summit of Mauna Kea, Hawaii. About 100 staff members (20 tour of duty staff, 70 locally hired staff, and 10 pos ...
... Subaru Telescope (observatory) is a branch of the National Astronomical Observatory of Japan operating the 8.2-meter (effective aperture) optical-infrared telescope “Subaru” located at the summit of Mauna Kea, Hawaii. About 100 staff members (20 tour of duty staff, 70 locally hired staff, and 10 pos ...
Infrared Astronomy
... Humans at normal body temperature, radiate most strongly in the infrared, which is definitely not seen by human eyes. The scientific discovery that the heat we all feel coming from the Sun is largely a radiation beyond the visible red colour of the solar spectrum was made by William Herschel in 1800 ...
... Humans at normal body temperature, radiate most strongly in the infrared, which is definitely not seen by human eyes. The scientific discovery that the heat we all feel coming from the Sun is largely a radiation beyond the visible red colour of the solar spectrum was made by William Herschel in 1800 ...
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... Cosmology is defined as “The study of the physical universe considered as a totality of phenomena in time and space.”[5] As one might expect from this lofty definition, the exploration of the nature of the universe has long been the province of poets, philosophers and religious thinkers – indeed, fo ...
... Cosmology is defined as “The study of the physical universe considered as a totality of phenomena in time and space.”[5] As one might expect from this lofty definition, the exploration of the nature of the universe has long been the province of poets, philosophers and religious thinkers – indeed, fo ...
Giant star seismology
... oscillations patterns, they were yet unable to fully constrain the internal structure of the stars (Miglio and Montalbán, 2005; Huber et al, 2011). Space-based instruments contributed to the progression of the field with the Hubble Space Telescope (Gilliland, 2008) and the star-tracker of the WIRE ...
... oscillations patterns, they were yet unable to fully constrain the internal structure of the stars (Miglio and Montalbán, 2005; Huber et al, 2011). Space-based instruments contributed to the progression of the field with the Hubble Space Telescope (Gilliland, 2008) and the star-tracker of the WIRE ...
The Day We Found the Universe
... the telescope's mirror was relatively small, it allowed him to estimate that there were tens of thousands of faint nebulae arrayed over the celestial sky, ten times more than had been known before. In the 1910s Lick astronomer Heber Curtis followed up on Keeler's ...
... the telescope's mirror was relatively small, it allowed him to estimate that there were tens of thousands of faint nebulae arrayed over the celestial sky, ten times more than had been known before. In the 1910s Lick astronomer Heber Curtis followed up on Keeler's ...
X-Ray Spectroscopy of Stars
... 4.2.2 Results from high-resolution spectra . . . . . . . . . . . . . . . . . . . . . . . 4.2.3 A new paradigm? . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.3 The case of early B-stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.4 Do Wolf-Rayet stars emi ...
... 4.2.2 Results from high-resolution spectra . . . . . . . . . . . . . . . . . . . . . . . 4.2.3 A new paradigm? . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.3 The case of early B-stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.4 Do Wolf-Rayet stars emi ...
The physics of line-driven winds of hot massive stars
... to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a million times that of our Sun, which is considered a nominal star. These stars are al ...
... to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a million times that of our Sun, which is considered a nominal star. These stars are al ...
Strongly suggested reading: The Milky Way`s stellar disk
... three-dimensional gravitational potential and by implication the dark-matter distribution in the Milky Way. A sequence of ongoing photometry and spectroscopy surveys has recently hundred-folded the number of stars with good distances, radial and transverse velocities, and abundance estimates; this o ...
... three-dimensional gravitational potential and by implication the dark-matter distribution in the Milky Way. A sequence of ongoing photometry and spectroscopy surveys has recently hundred-folded the number of stars with good distances, radial and transverse velocities, and abundance estimates; this o ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.