Subatomic particle processes within neutron stars
... The idea of “strangeness” of matter is older than someone might think. It has been suggested already back in 1970 by a number of researchers that neutrons, protons plus the heavier constitutes (∆, Σ, Λ, Ξ) can melt, creating the quark-gluon plasma state. Evidence of the creation of such matter in th ...
... The idea of “strangeness” of matter is older than someone might think. It has been suggested already back in 1970 by a number of researchers that neutrons, protons plus the heavier constitutes (∆, Σ, Λ, Ξ) can melt, creating the quark-gluon plasma state. Evidence of the creation of such matter in th ...
Elliptical galaxies
... plane relation (last panel) They express some fundamental property of E galaxies. They can be understood partially from the virial theorem ...
... plane relation (last panel) They express some fundamental property of E galaxies. They can be understood partially from the virial theorem ...
Mapping of the extinction in giant molecular clouds using optical star
... which depends only on one or two free parameters. The mass spectrum of interstellar clouds can also be understood assuming a fractal structure (Elmegreen & Falgarone, 1996). Larson (1995) went further, showing that the Taurus cloud also presents a fractal structure in the distribution of its young s ...
... which depends only on one or two free parameters. The mass spectrum of interstellar clouds can also be understood assuming a fractal structure (Elmegreen & Falgarone, 1996). Larson (1995) went further, showing that the Taurus cloud also presents a fractal structure in the distribution of its young s ...
Supernovae and Gamma-Ray Bursts (draft)
... can be deposited just below the accretion shock and be allowed to accumulate till enough energy is available to drive an explosion. In the presently favoured model of delayed neutrino-driven explosions, this may require more than 500 ms, which is extremely long compared to the dynamical timescale of ...
... can be deposited just below the accretion shock and be allowed to accumulate till enough energy is available to drive an explosion. In the presently favoured model of delayed neutrino-driven explosions, this may require more than 500 ms, which is extremely long compared to the dynamical timescale of ...
Galaxies
... 1. Who first calibrated the Cepheid variable stars for use in determining distance? a. Henrietta Leavitt b. Edwin Hubble c. John Glenn d. Carl Sagan e. Harlow Shapley 2. Which of the following is not a characteristic of the stars of the disk component of our galaxy? a. circular orbits b. randomly in ...
... 1. Who first calibrated the Cepheid variable stars for use in determining distance? a. Henrietta Leavitt b. Edwin Hubble c. John Glenn d. Carl Sagan e. Harlow Shapley 2. Which of the following is not a characteristic of the stars of the disk component of our galaxy? a. circular orbits b. randomly in ...
![arXiv:1007.5481v1 [astro-ph.EP] 30 Jul 2010](http://s1.studyres.com/store/data/016640559_1-8bc20118c4d48efd5cfe1f2b10a85bec-300x300.png)
arXiv:1007.5481v1 [astro-ph.EP] 30 Jul 2010
... fiber-fed from the Cassegrain focus of the 3.6 m telescope at La Silla Observatory, Chile (Mayor et al. 2003). Fifteen spectra with a spectral resolution R ≈ 115 000 were obtained using exposure times of 3600 s, and setting one of the two available fibers on the sky in order to monitor the presence ...
... fiber-fed from the Cassegrain focus of the 3.6 m telescope at La Silla Observatory, Chile (Mayor et al. 2003). Fifteen spectra with a spectral resolution R ≈ 115 000 were obtained using exposure times of 3600 s, and setting one of the two available fibers on the sky in order to monitor the presence ...
Sec 30.1 - Highland High School
... What method did astronomers use to determine the shape of the Milky Way galaxy? a. measuring X-ray emissions b. observing Cepheid variables c. mapping the galaxy with radio waves d. sending out long-range space probes ...
... What method did astronomers use to determine the shape of the Milky Way galaxy? a. measuring X-ray emissions b. observing Cepheid variables c. mapping the galaxy with radio waves d. sending out long-range space probes ...
MS Word
... During an impact, the energy is transferred to the target surface, breaking up rock and moving the particles around. You can calculate the kinetic energy in the craters you’ve already made by plugging the velocity and mass into the formula above. As long as your mass is in grams and your velocity in ...
... During an impact, the energy is transferred to the target surface, breaking up rock and moving the particles around. You can calculate the kinetic energy in the craters you’ve already made by plugging the velocity and mass into the formula above. As long as your mass is in grams and your velocity in ...
Pop Quiz Question
... Which is the largest star: A. a M7 I star B. a F4IV star C. a AIV star D. a O2 II star ...
... Which is the largest star: A. a M7 I star B. a F4IV star C. a AIV star D. a O2 II star ...
astro-ph/9410035 PDF
... path of the particles is much smaller than the macroscopic scales of interest), but \bulk viscosity" can be substantially more subtle and complicated, as should become clear below, particularly in x3.1. The contraction of a neutron star due to spin-down also causes adiabatic heating. However, the ad ...
... path of the particles is much smaller than the macroscopic scales of interest), but \bulk viscosity" can be substantially more subtle and complicated, as should become clear below, particularly in x3.1. The contraction of a neutron star due to spin-down also causes adiabatic heating. However, the ad ...
Lecture 3 - University of Washington
... • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long enough time to be consisten ...
... • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long enough time to be consisten ...
Making Visual Estimates
... Variable and comparison stars Look at the example below. The variable is shown between the four focus lines. The magnitudes of the comparison (“comp”) stars are shown on the chart next to the stars (64,51,91, etc.). ...
... Variable and comparison stars Look at the example below. The variable is shown between the four focus lines. The magnitudes of the comparison (“comp”) stars are shown on the chart next to the stars (64,51,91, etc.). ...
Astrophysics
... uses hydrodynamic simulations to study the evolution of SNRs, the role of instabilities in mixing heavyelement ejecta with circumstellar gas, and the formation of large-scale asymmetries. Prof. Reynolds models synchrotron emission at radio and X-ray wavelengths from shell SNRs as well as from pulsar ...
... uses hydrodynamic simulations to study the evolution of SNRs, the role of instabilities in mixing heavyelement ejecta with circumstellar gas, and the formation of large-scale asymmetries. Prof. Reynolds models synchrotron emission at radio and X-ray wavelengths from shell SNRs as well as from pulsar ...
Here
... pixels. It is possible to do photometry (the image recorded is then a portion of the sky/star/galaxy) or spectroscopy (the light is dispersed by using a grating into its colors). There are some common problems with CCDs, which need to be taken into account in every observational program: -read-out n ...
... pixels. It is possible to do photometry (the image recorded is then a portion of the sky/star/galaxy) or spectroscopy (the light is dispersed by using a grating into its colors). There are some common problems with CCDs, which need to be taken into account in every observational program: -read-out n ...
Equations of State for White Dwarfs Elena Heikkilä Kandidaatin
... White dwarfs are compact objects — they no longer burn nuclear fuel, but they are cooling by radiating thermal energy. An isolated white dwarf star cools to zero temperature, since it has no internal sources of energy. The pressure associated with matter at T = 0 supports the star against the gravit ...
... White dwarfs are compact objects — they no longer burn nuclear fuel, but they are cooling by radiating thermal energy. An isolated white dwarf star cools to zero temperature, since it has no internal sources of energy. The pressure associated with matter at T = 0 supports the star against the gravit ...
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.