Research Report for 2015/2016
... MS thesis described numerical work related to a new experimental design of a planetary magnetosphere. We obtained the first data with this platform last year, and have also initiated a new series of experiments in collaboration with C. Kuranz at the University of Michigan to study magnetized accreti ...
... MS thesis described numerical work related to a new experimental design of a planetary magnetosphere. We obtained the first data with this platform last year, and have also initiated a new series of experiments in collaboration with C. Kuranz at the University of Michigan to study magnetized accreti ...
Plotting the Rotation Curve of M31
... Questions to ask the class before the activity: What is the Universe composed of? Answer: energy, luminous matter, dark matter, dark energy. What are galaxies? Answer: large collections of stars. They vary in their morphology and stellar composition i.e. ellipticals are red and contain older stars t ...
... Questions to ask the class before the activity: What is the Universe composed of? Answer: energy, luminous matter, dark matter, dark energy. What are galaxies? Answer: large collections of stars. They vary in their morphology and stellar composition i.e. ellipticals are red and contain older stars t ...
MPhil Thesis - Final - Suzanne Knight
... outcomes of the CNO cycle is the conversion of almost all central !"C into !"N. ...
... outcomes of the CNO cycle is the conversion of almost all central !"C into !"N. ...
Telluric Line Removal in Astrophysical Spectroscopy
... 2, the telluric template has lines that are stronger than the observation, creating false features on the quotient due to overcorrection. In plot 3, an absorption feature in the template is stellar in origin, which results in removing the feature from the observation and actually creating a false fe ...
... 2, the telluric template has lines that are stronger than the observation, creating false features on the quotient due to overcorrection. In plot 3, an absorption feature in the template is stellar in origin, which results in removing the feature from the observation and actually creating a false fe ...
Jul y 10-12,
... center with Chandra, following up XRTs with HST; 4σ B magnitude limits for counterparts are ∼ 26 − 29. We obtain period estimates for each XRT for both neutron star and BH accretors. These M31 XRTs appear to be somewhat skewed towards shorter periods than XRTs in the Milky Way. ...
... center with Chandra, following up XRTs with HST; 4σ B magnitude limits for counterparts are ∼ 26 − 29. We obtain period estimates for each XRT for both neutron star and BH accretors. These M31 XRTs appear to be somewhat skewed towards shorter periods than XRTs in the Milky Way. ...
Stars: Stellar Evol & “death” Galaxies Astronomy 1 — Elementary Astronomy
... deduced that they were observing very rapidly rotating neutron stars -pulsars. ...
... deduced that they were observing very rapidly rotating neutron stars -pulsars. ...
Strongly suggested reading: The stellar halo of the Galaxy
... stellar halo that (hopefully) provide the most direct clues to its evolutionary path. The stellar halo is arguably the component that contains the most useful information about the evolutionary history of the Galaxy. This is because the most metal-poor stars in the Galaxy and possibly some of the ol ...
... stellar halo that (hopefully) provide the most direct clues to its evolutionary path. The stellar halo is arguably the component that contains the most useful information about the evolutionary history of the Galaxy. This is because the most metal-poor stars in the Galaxy and possibly some of the ol ...
Acta Polytechnica
... This is the most energetic event in the Universe since the Big Bang. If two such objects collide with each other, a huge amount of energy may be released and a certain fraction is expected to heat the gas and accelerate particles through shock waves, and induce bulk and turbulent gas motions. Signat ...
... This is the most energetic event in the Universe since the Big Bang. If two such objects collide with each other, a huge amount of energy may be released and a certain fraction is expected to heat the gas and accelerate particles through shock waves, and induce bulk and turbulent gas motions. Signat ...
black hole masses and host galaxy evolution of radio
... estimates with various indirect methods are somewhat uncertain and more accurate data for various types of AGNs at various redshift ranges are needed. Studies with Hubble Space Telescope (HST ) data showed that host galaxies of bright quasars are typically massive ellipticals with a de Vaucouleurs p ...
... estimates with various indirect methods are somewhat uncertain and more accurate data for various types of AGNs at various redshift ranges are needed. Studies with Hubble Space Telescope (HST ) data showed that host galaxies of bright quasars are typically massive ellipticals with a de Vaucouleurs p ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
Determination of accurate stellar radial
... Following the general introduction of efficient CCD detectors in astronomy, digital cross-correlation has become a standard technique for determination of stellar radial velocities. In this method the recorded stellar spectrum, after suitable calibration and normalisation, is correlated with a digit ...
... Following the general introduction of efficient CCD detectors in astronomy, digital cross-correlation has become a standard technique for determination of stellar radial velocities. In this method the recorded stellar spectrum, after suitable calibration and normalisation, is correlated with a digit ...
the structure of the local interstellar medium. v. electron densities
... (e.g., Oliveira et al. 2003). This collection of new, high spectral resolution UV observations of nearby stars presents an opportunity to greatly expand the number of LISM electron density measurements and probe the ionization structure of our most immediate interstellar environment. 2. OBSERVATIONS ...
... (e.g., Oliveira et al. 2003). This collection of new, high spectral resolution UV observations of nearby stars presents an opportunity to greatly expand the number of LISM electron density measurements and probe the ionization structure of our most immediate interstellar environment. 2. OBSERVATIONS ...
2. The X-ray-Radio correlation for bulgeless galaxies
... as been zoomed to allow for a better visualization of the sources...............................................................45 Fig. 22: Flux distribution for the radio-detected sources as captured by the VLA-COSMOS Large Survey. Like in the previous instances, the flux is set to a logarithmic sc ...
... as been zoomed to allow for a better visualization of the sources...............................................................45 Fig. 22: Flux distribution for the radio-detected sources as captured by the VLA-COSMOS Large Survey. Like in the previous instances, the flux is set to a logarithmic sc ...
Edmund C. Stoner and the discovery of the maximum mass of white
... exclusion principle could be applied to solve a major puzzle, the origin of the extreme high density of white dwarfs ix x, which could not be explained by classical physics. Eddington expressed this puzzle as follows: `` I do not see how a star which has once got into this compressed state is ever g ...
... exclusion principle could be applied to solve a major puzzle, the origin of the extreme high density of white dwarfs ix x, which could not be explained by classical physics. Eddington expressed this puzzle as follows: `` I do not see how a star which has once got into this compressed state is ever g ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Evolution and colors of helium-core white dwarf stars with high
... white dwarfs offers the possibility of constraining globular cluster dynamics and evolution (Moehler & Bono 2008). The possible detection of single low-mass white dwarfs in NGC 6791, one of the oldest (> ∼8 Gyr) and most metal-rich ([Fe/H] ≈ +0.4) open clusters in our Galaxy (Origlia et al. 2006), ha ...
... white dwarfs offers the possibility of constraining globular cluster dynamics and evolution (Moehler & Bono 2008). The possible detection of single low-mass white dwarfs in NGC 6791, one of the oldest (> ∼8 Gyr) and most metal-rich ([Fe/H] ≈ +0.4) open clusters in our Galaxy (Origlia et al. 2006), ha ...
20_Testbank
... the Milky Way. Therefore, they serve as a bridge between us and standard candles in other galaxies. Once we determine the distance to another galaxy for which we have observed a whitedwarf supernova, we then can calibrate the average luminosity of white-dwarf supernovae. White-dwarf supernovae and C ...
... the Milky Way. Therefore, they serve as a bridge between us and standard candles in other galaxies. Once we determine the distance to another galaxy for which we have observed a whitedwarf supernova, we then can calibrate the average luminosity of white-dwarf supernovae. White-dwarf supernovae and C ...
Seminar Outburst of Comet 17P/Holmes
... nucleus together with dust and rocky particles. Material ejected from the nucleus forms sparse atmosphere which is called a coma. At some distance from the nucleus the coma becomes so tenuous that particles in it become unbound and they interact only with solar radiation. Neutral (uncharged) particl ...
... nucleus together with dust and rocky particles. Material ejected from the nucleus forms sparse atmosphere which is called a coma. At some distance from the nucleus the coma becomes so tenuous that particles in it become unbound and they interact only with solar radiation. Neutral (uncharged) particl ...
Article PDF - IOPscience
... Received 2013 August 12; accepted 2013 August 28; published 2013 September 12 ...
... Received 2013 August 12; accepted 2013 August 28; published 2013 September 12 ...
Hewitt/Lyons/Suchocki/Yeh, Conceptual Integrated Science
... Note: positions that form a main sequence for average stars, and exotic stars above or below the main sequence. The H-R diagram is to an astronomer what the Periodic Table is to a ...
... Note: positions that form a main sequence for average stars, and exotic stars above or below the main sequence. The H-R diagram is to an astronomer what the Periodic Table is to a ...
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.