ph600-12 - University of Kent
... source and analysed in order to generate, in an original way, fresh evidence for or against the available solutions. The study will then consider new or hybrid solutions before considering how these can be tested. The relevance of new ground-based telescopes or space missions will be discussed. ...
... source and analysed in order to generate, in an original way, fresh evidence for or against the available solutions. The study will then consider new or hybrid solutions before considering how these can be tested. The relevance of new ground-based telescopes or space missions will be discussed. ...
Ionized gas discs in elliptical and S0 galaxies at z < 1
... the cessation of star formation, but also with the time of accretion into the cluster, clearly indicating that the transformation of spirals to S0s is accelerated by cluster environment. All of the above-mentioned studies however have been done at low redshift. In this paper, we present, for the fir ...
... the cessation of star formation, but also with the time of accretion into the cluster, clearly indicating that the transformation of spirals to S0s is accelerated by cluster environment. All of the above-mentioned studies however have been done at low redshift. In this paper, we present, for the fir ...
Test 4 Review Clicker Questions
... and grew. d) spiral density waves formed first. e) the bar in the bulge formed first. ...
... and grew. d) spiral density waves formed first. e) the bar in the bulge formed first. ...
The Search for the Earliest Galaxies
... where small objects merged to form larger ones through collision and agglomeration. The findings from the HUDF09 survey support this hierarchical model of galaxy assembly. Still, there is a big mystery that remains unsolved. Current galaxy counts in the era between 400 million and 900 million years ...
... where small objects merged to form larger ones through collision and agglomeration. The findings from the HUDF09 survey support this hierarchical model of galaxy assembly. Still, there is a big mystery that remains unsolved. Current galaxy counts in the era between 400 million and 900 million years ...
The Big Bang
... are usually observed to be regular systems that don’t look particularly disturbed. Most of the small “modern day” galaxies look quite irregular. In very rough numbers, “large” galaxies have 10 billion stars or more, “small galaxies” have 1 million to 100 million stars. ...
... are usually observed to be regular systems that don’t look particularly disturbed. Most of the small “modern day” galaxies look quite irregular. In very rough numbers, “large” galaxies have 10 billion stars or more, “small galaxies” have 1 million to 100 million stars. ...
Dark matter scaling relations and the assembly epoch of Coma early
... Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galaxies become bluer towards the outer parts and B-band light profiles are slightly shallower than R-band profiles. Likewise, mass profiles of galaxies are generally shallower th ...
... Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galaxies become bluer towards the outer parts and B-band light profiles are slightly shallower than R-band profiles. Likewise, mass profiles of galaxies are generally shallower th ...
REVIEW Numerical Star-Formation Studies— A Status Report
... molecules. Star formation appears to occur exclusively within this molecular phase of the ISM. Molecular hydrogen is a homonuclear molecule, so its dipole moment vanishes and it radiates extremely weakly. Direct detection of cold interstellar H2 is generally possibly only through ultraviolet absorpt ...
... molecules. Star formation appears to occur exclusively within this molecular phase of the ISM. Molecular hydrogen is a homonuclear molecule, so its dipole moment vanishes and it radiates extremely weakly. Direct detection of cold interstellar H2 is generally possibly only through ultraviolet absorpt ...
Comparison of low- and high-mass star formation
... to competitive accretion. One may plausibly identify the dense filament in the early phase and the dense region at the bottom of the global gravitational potential well in the late phase as a McKee–Tan core (McKee & Tan 2003). However, the “cores” so identified are transient objects that are not in ...
... to competitive accretion. One may plausibly identify the dense filament in the early phase and the dense region at the bottom of the global gravitational potential well in the late phase as a McKee–Tan core (McKee & Tan 2003). However, the “cores” so identified are transient objects that are not in ...
Giant Molecular Clouds in Local Group Galaxies
... is a good value to use in most galaxies (except the SMC) if the GMCs are virialized. However, if the clouds are only marginally self-gravitating, as appears to be the case judging from their appearance, half the virial value may be more appropriate. There is no clear trend of XCO with metallicity. T ...
... is a good value to use in most galaxies (except the SMC) if the GMCs are virialized. However, if the clouds are only marginally self-gravitating, as appears to be the case judging from their appearance, half the virial value may be more appropriate. There is no clear trend of XCO with metallicity. T ...
16_Testbank
... D) 30 E) 200 Answer: E 37) Which of the following discoveries, if they existed, would necessitate a reevaluation of our ideas of stellar formation? A) a cluster of stars that appeared to be 13 billion years old B) a 100-solar-mass star C) a 0.01-solar-mass star D) a molecular cloud without any stars ...
... D) 30 E) 200 Answer: E 37) Which of the following discoveries, if they existed, would necessitate a reevaluation of our ideas of stellar formation? A) a cluster of stars that appeared to be 13 billion years old B) a 100-solar-mass star C) a 0.01-solar-mass star D) a molecular cloud without any stars ...
Summary of Talks at Growing Black Holes 2004 in Garching
... to estimates of quasar lifetimes. At z < 2.5, SDSS clustering scale is about 7 Mpc. There is now preliminary, tentative evidence for correlation length to increase with redshift. Spectra of emission lines in high z quasars & Continuum shape consistent with lower z objects -> implication : rapid ch ...
... to estimates of quasar lifetimes. At z < 2.5, SDSS clustering scale is about 7 Mpc. There is now preliminary, tentative evidence for correlation length to increase with redshift. Spectra of emission lines in high z quasars & Continuum shape consistent with lower z objects -> implication : rapid ch ...
Planet formation in the habitable zone of alpha Centauri B
... τdiss = 105 years. The dissipation is started at 104 years, the end of our nominal run, when all orbits have reached their size-dependent alignment in the HZ. Fig.3 shows the dynamical state of the system after 2τdiss = 2x105 years and clearly illustrates the efficient re-phasing of all orbits, whic ...
... τdiss = 105 years. The dissipation is started at 104 years, the end of our nominal run, when all orbits have reached their size-dependent alignment in the HZ. Fig.3 shows the dynamical state of the system after 2τdiss = 2x105 years and clearly illustrates the efficient re-phasing of all orbits, whic ...
Dark Matter Search
... • As we start the third year of operations, we have only scratched the surface of what the Fermi Gamma-ray Space Telescope can do. – The gamma-ray sky is changing every day, so there is always something new to learn about the extreme Universe. ...
... • As we start the third year of operations, we have only scratched the surface of what the Fermi Gamma-ray Space Telescope can do. – The gamma-ray sky is changing every day, so there is always something new to learn about the extreme Universe. ...
The Submillimeter Frontier: A Space Science Imperative
... of newly synthesized heavy elements. Galaxies grow by collisions and absorption of smaller fragments, with a rate governed by the statistics of the primordial density fluctuations and their growth. Many are very dusty, with star formation obscured by very local dust from young hot stars and supernov ...
... of newly synthesized heavy elements. Galaxies grow by collisions and absorption of smaller fragments, with a rate governed by the statistics of the primordial density fluctuations and their growth. Many are very dusty, with star formation obscured by very local dust from young hot stars and supernov ...
Discovery of a bright quasar without a massive
... As a complementary approach, avoiding uncertainties related to the black hole mass estimates, we compare directly our upper limits to the magnitudes measured for typical quasar host galaxies. We use the HST sample of 17 quasar host galaxies from Floyd et al.8. After conversion of their values to our ...
... As a complementary approach, avoiding uncertainties related to the black hole mass estimates, we compare directly our upper limits to the magnitudes measured for typical quasar host galaxies. We use the HST sample of 17 quasar host galaxies from Floyd et al.8. After conversion of their values to our ...
PPT
... – External to system UV from hot, high-mass O stars X-rays from neighbouring stars X-rays from shocked winds from high-mass stars? Kevin Briggs, PSI/ETH ...
... – External to system UV from hot, high-mass O stars X-rays from neighbouring stars X-rays from shocked winds from high-mass stars? Kevin Briggs, PSI/ETH ...
Does feedback help or hinder star formation? The effect of
... molecular weight is calculated from the species abundances, giving a value µ ∼1.2. The radiative cooling then extends down to 10 K, which is the temperature of the giant molecular clouds. For our idealised cloud simulations, the box size has a side of 200 pc, covered by a 1283 root grid and an addit ...
... molecular weight is calculated from the species abundances, giving a value µ ∼1.2. The radiative cooling then extends down to 10 K, which is the temperature of the giant molecular clouds. For our idealised cloud simulations, the box size has a side of 200 pc, covered by a 1283 root grid and an addit ...
Interpretation of the Helix Planetary Nebula using Hydro
... or PFPs) that form larger planets and finally stars as binaries. Planetary nebulae are not just brief puffs of illuminated gas and dust from dying stars in a vacuum, but are manifestations of the thirty million primordial dark matter planets that surround every star. Whenever a central star gets hot ...
... or PFPs) that form larger planets and finally stars as binaries. Planetary nebulae are not just brief puffs of illuminated gas and dust from dying stars in a vacuum, but are manifestations of the thirty million primordial dark matter planets that surround every star. Whenever a central star gets hot ...
Age Distributions of Low Mass Stars in the Rho Ophiucus Molecular
... The Rho Ophiuchi (Rho Oph) cloud complex is a cluster of star-forming molecular clouds in the constellation Ophiuchus. The coordinates are right ascension of 16h 28m 06s and declination of –24d 32.5s [1]. This makes it accessible from both hemispheres. It consists of two main regions of dense gas an ...
... The Rho Ophiuchi (Rho Oph) cloud complex is a cluster of star-forming molecular clouds in the constellation Ophiuchus. The coordinates are right ascension of 16h 28m 06s and declination of –24d 32.5s [1]. This makes it accessible from both hemispheres. It consists of two main regions of dense gas an ...
$^{13} $ CO/C $^{18} $ O Gradients Across the Disks of Nearby
... the other targets with resolved gradients show decreasing 13 CO/C18 O with increasing ΣSFR . As discussed below, the sense of this trend is what is expected if massive star nucleosynthesis alters the isotopic abundances, but it might also reflect optical depth effects. In either case, as we sort our ...
... the other targets with resolved gradients show decreasing 13 CO/C18 O with increasing ΣSFR . As discussed below, the sense of this trend is what is expected if massive star nucleosynthesis alters the isotopic abundances, but it might also reflect optical depth effects. In either case, as we sort our ...
Article PDF - IOPscience
... surface brightness. It is not correlated with linear size. Gas fraction varies with luminosity and surface brightness at the same rate, indicating evolution at Ðxed size. Dim galaxies are clearly less evolved than bright ones, having consumed only D1 of their gas. This 2 reservoirs. These resolves t ...
... surface brightness. It is not correlated with linear size. Gas fraction varies with luminosity and surface brightness at the same rate, indicating evolution at Ðxed size. Dim galaxies are clearly less evolved than bright ones, having consumed only D1 of their gas. This 2 reservoirs. These resolves t ...
THE DYNAMICAL STRUCTURE AND EVOLUTION OF GIANT
... vicinity, the total interstellar pressure is about 2:8 104 K cm;3 , which balances the weight of the ISM 14]. Of this, about 0:7 104 K cm;3 is due to cosmic rays since they pervade both the ISM and a molecular cloud, they do not contribute to the support of a cloud and may be neglected. The ma ...
... vicinity, the total interstellar pressure is about 2:8 104 K cm;3 , which balances the weight of the ISM 14]. Of this, about 0:7 104 K cm;3 is due to cosmic rays since they pervade both the ISM and a molecular cloud, they do not contribute to the support of a cloud and may be neglected. The ma ...
FREE Sample Here
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
Astronomy and the Coal Age of Alabama
... The sky is like a time machine. Light travels in vacuum at finite speed, 186,272 miles per second. In a year, a beam of light travels one light year, or 6 trillion miles. This means that the farther out in space we look, the farther back in time we see. The Minkin site is 310 Myr old. Sunlight that ...
... The sky is like a time machine. Light travels in vacuum at finite speed, 186,272 miles per second. In a year, a beam of light travels one light year, or 6 trillion miles. This means that the farther out in space we look, the farther back in time we see. The Minkin site is 310 Myr old. Sunlight that ...
The formation of spiral galaxies - Case Western Reserve University
... halo, so an unphysically low concentration in the current dark matter halo implies an antecedent primordial halo whose concentration is still less consistent with cold dark matter (CDM). These are galaxies for which feedback or some other mechanism must be invoked in order to rearrange the primord ...
... halo, so an unphysically low concentration in the current dark matter halo implies an antecedent primordial halo whose concentration is still less consistent with cold dark matter (CDM). These are galaxies for which feedback or some other mechanism must be invoked in order to rearrange the primord ...