Gas Evolution in Disk Galaxies
... to understand the evolution course of galaxies over cosmological time scales. Hubble’s next celebrated discovery, Hubble’s law (Hubble 1929), was empirically derived as v = H0 D, with v being the recession velocity, the Hubble constant H0 (73.5 ± 3.2 km s−1 Mpc−1 derived from the five-year WMAP, 200 ...
... to understand the evolution course of galaxies over cosmological time scales. Hubble’s next celebrated discovery, Hubble’s law (Hubble 1929), was empirically derived as v = H0 D, with v being the recession velocity, the Hubble constant H0 (73.5 ± 3.2 km s−1 Mpc−1 derived from the five-year WMAP, 200 ...
Search For Gas Giants Around Late-m Dwarfs - STARS
... whom I spent countless number of hours on phone. This thesis would not have been complete without the help, guidance and support of Dr. Michele M. Montgomery. Discussions with her have greatly helped me in my work. Thank you to the Physics staff, Mike Jimenez, Felix Ayala, Monika Crittenden, Jessica ...
... whom I spent countless number of hours on phone. This thesis would not have been complete without the help, guidance and support of Dr. Michele M. Montgomery. Discussions with her have greatly helped me in my work. Thank you to the Physics staff, Mike Jimenez, Felix Ayala, Monika Crittenden, Jessica ...
THE COBE DIRBE POINT SOURCE CATALOG
... For each wavelength, three different confusion flags may be set in the DIRBE Point Source Catalog (see Table 2 for a summary of the flags and Table 3 for some basic statistics on the DIRBE Catalog, including statistics on flagging and number of sources detected above 3 at each wavelength). The fir ...
... For each wavelength, three different confusion flags may be set in the DIRBE Point Source Catalog (see Table 2 for a summary of the flags and Table 3 for some basic statistics on the DIRBE Catalog, including statistics on flagging and number of sources detected above 3 at each wavelength). The fir ...
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 ...
the Ëg infrared search for extraterrestrial civilizations with large
... Most relevant to the present paper are the parameters γ (waste heat luminosity, expressed as a fraction of the starlight available to the civilization) and Twaste , the characteristic temperature of the waste heat (which dictates its infrared colors). For values of Twaste in the 100–600 K range, val ...
... Most relevant to the present paper are the parameters γ (waste heat luminosity, expressed as a fraction of the starlight available to the civilization) and Twaste , the characteristic temperature of the waste heat (which dictates its infrared colors). For values of Twaste in the 100–600 K range, val ...
H i AND CO IN BLUE COMPACT DWARF GALAXIES: HARO 2 AND
... (Papaderos et al. 1996; Östlin 2000; Tosi 2001). This poses some interesting questions regarding the production and possible loss of heavy elements. Recent X-ray observations with the Chandra X-Ray Observatory seem to indicate that in starbursting dwarf galaxies, such as NGC 1569 and NGC 3077 (Mart ...
... (Papaderos et al. 1996; Östlin 2000; Tosi 2001). This poses some interesting questions regarding the production and possible loss of heavy elements. Recent X-ray observations with the Chandra X-Ray Observatory seem to indicate that in starbursting dwarf galaxies, such as NGC 1569 and NGC 3077 (Mart ...
Legends Night Sky Orion
... To find Ursa Minor (the Little Dipper) using Ursa Major (the Big Dipper) as your guide.): - Follow the two stars at the end of the bowl in a straight line for approximately 30 degrees (or three fists held at arm’s length) and you will end up on the north star. - Polaris, the North Star, is the star ...
... To find Ursa Minor (the Little Dipper) using Ursa Major (the Big Dipper) as your guide.): - Follow the two stars at the end of the bowl in a straight line for approximately 30 degrees (or three fists held at arm’s length) and you will end up on the north star. - Polaris, the North Star, is the star ...
Spherical planetary nebulae
... these PNe interacted with a stellar companion via a common envelope phase. (iv) Elliptical PNe. By elliptical alone, I refer to moderate elliptical PNe which show only small departure from sphericity. In S97 the progenitors of these PNe were assumed to have interacted with substellar objects, but no ...
... these PNe interacted with a stellar companion via a common envelope phase. (iv) Elliptical PNe. By elliptical alone, I refer to moderate elliptical PNe which show only small departure from sphericity. In S97 the progenitors of these PNe were assumed to have interacted with substellar objects, but no ...
The effect of dark matter capture on binary stars
... This work has led to a number of interesting conclusions: (1) Binary stars, due to their orbital motion, can produce more collisions that result in initially bound orbits. However, the gravitational interaction with two masses quickly scatters nearly all WIMPs out of the system. The few that survive ...
... This work has led to a number of interesting conclusions: (1) Binary stars, due to their orbital motion, can produce more collisions that result in initially bound orbits. However, the gravitational interaction with two masses quickly scatters nearly all WIMPs out of the system. The few that survive ...
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... Numerical 3D simulations enable one to compute directly the excitation rates of p-modes for stars with various temperatures and luminosities. For instance this was already undertaken for the Sun by Stein & Nordlund (2001) using the numerical approach introduced in Nordlund & Stein (2001). Such calcu ...
... Numerical 3D simulations enable one to compute directly the excitation rates of p-modes for stars with various temperatures and luminosities. For instance this was already undertaken for the Sun by Stein & Nordlund (2001) using the numerical approach introduced in Nordlund & Stein (2001). Such calcu ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
β Relation for Local Galaxies
... lost to dust attenuation and being re-emitted in the infrared (IR). UV wavelengths, while the most susceptible to the effects of dust, provide insights on the young stellar populations, while longer wavelengths provide information on the older and more evolved stellar populations. Observations from ...
... lost to dust attenuation and being re-emitted in the infrared (IR). UV wavelengths, while the most susceptible to the effects of dust, provide insights on the young stellar populations, while longer wavelengths provide information on the older and more evolved stellar populations. Observations from ...
Type II SuperNova - University of Dayton
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
THE CHEMICAL COMPOSITION AND AGE OF THE METAL
... studies have attempted to understand the changing nature of element production as a function of metallicity and time throughout the Galaxy’s history (see Wheeler, Sneden, & Truran 1989 and references therein). Thus, while barium appears to be synthesized by the r-process at earliest times, this elem ...
... studies have attempted to understand the changing nature of element production as a function of metallicity and time throughout the Galaxy’s history (see Wheeler, Sneden, & Truran 1989 and references therein). Thus, while barium appears to be synthesized by the r-process at earliest times, this elem ...
Methanol Masers in the NGC6334F Star Forming Region
... • These models suggest the following physical parameters for the masing region : nH2 = 106 cm-3, Tgas = 30K, Tdust = 150K, beaming factor around 10. • These parameters are all very plausible for young highmass star formation regions. • The modeling assumes that the emission from the different transi ...
... • These models suggest the following physical parameters for the masing region : nH2 = 106 cm-3, Tgas = 30K, Tdust = 150K, beaming factor around 10. • These parameters are all very plausible for young highmass star formation regions. • The modeling assumes that the emission from the different transi ...
A spectroscopic study of detached binary systems using precise radial velocities
... orbits, whilst others result from much more active processes, such as mass exchange leading to intense radiation emissions. A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the ...
... orbits, whilst others result from much more active processes, such as mass exchange leading to intense radiation emissions. A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the ...
Rich
... vary from galaxy to galaxy. • Opportunity: Galex grism mode in Far-UV (FUV) used to discover the first known sample of low redshift LAE galaxies. Instead of studying LAEs at z~4, study them at z~0.3 • Goal: Analyze photometry and spectroscopy of a local z~0.3 sample of ~76 LAEs and 107 non-LAEs to : ...
... vary from galaxy to galaxy. • Opportunity: Galex grism mode in Far-UV (FUV) used to discover the first known sample of low redshift LAE galaxies. Instead of studying LAEs at z~4, study them at z~0.3 • Goal: Analyze photometry and spectroscopy of a local z~0.3 sample of ~76 LAEs and 107 non-LAEs to : ...
Review of asymmetric dark matter
... In most ADM models, the number density of DM particles is comparable to that of baryons. The observed relation of Eq. (1.1) then requires the DM particle mass to be typically, though not exclusively, in the 1-15 GeV regime, with the precise figure depending on details of the model, such as its DM ba ...
... In most ADM models, the number density of DM particles is comparable to that of baryons. The observed relation of Eq. (1.1) then requires the DM particle mass to be typically, though not exclusively, in the 1-15 GeV regime, with the precise figure depending on details of the model, such as its DM ba ...
Lya escape from z~ 0.03 star-forming galaxies: the dominant role of
... (Charlot & Fall 1993; Valls-Gabaud 1993; Verhamme et al. 2008). The above predictions do not account for the underlying stellar contribution at Lyα. This contribution is not a concern in galaxies dominated by populations of O and early B stars. For reference, the mean Lyα equivalent width of the eig ...
... (Charlot & Fall 1993; Valls-Gabaud 1993; Verhamme et al. 2008). The above predictions do not account for the underlying stellar contribution at Lyα. This contribution is not a concern in galaxies dominated by populations of O and early B stars. For reference, the mean Lyα equivalent width of the eig ...
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.