Ultraluminous X-ray Sources in Andromeda Galaxy
... Begelman (2001). The author suggested non-linear plane wave solutions, in a steady state, in which radiation pressure and magnetic tension forces are dynamically coupled. The main point in the context of ULXs is that the total flux observed from such an atmosphere can exceed the Eddington limit with ...
... Begelman (2001). The author suggested non-linear plane wave solutions, in a steady state, in which radiation pressure and magnetic tension forces are dynamically coupled. The main point in the context of ULXs is that the total flux observed from such an atmosphere can exceed the Eddington limit with ...
doc - Pocket Stars
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
8th Ed【CH13】
... which confirms the expectation of slope = 2/3 based on the above equation. (c) And the 1.01 intercept corresponds to the term 1/3 log (Mo/M) which implies ...
... which confirms the expectation of slope = 2/3 based on the above equation. (c) And the 1.01 intercept corresponds to the term 1/3 log (Mo/M) which implies ...
On the problem of very energetic flares in binary systems
... On the other hand, stellar flares can be several orders of magnitude more energetic than their solar counterparts which does raise the problem of finding a capable energy source to explain them (Byrne 1990). Stellar flares have generally been interpreted as scaled up versions of solar flares so that ...
... On the other hand, stellar flares can be several orders of magnitude more energetic than their solar counterparts which does raise the problem of finding a capable energy source to explain them (Byrne 1990). Stellar flares have generally been interpreted as scaled up versions of solar flares so that ...
Results from the search for tidal disruption flares in the GALEX Deep
... Why Search For Tidal Disruption Events? • They are an unambiguous probe for supermassive black holes lurking in the nuclei of normal galaxies. • The luminosity, temperature, and decay of the flare is dependent on the mass and spin of the black hole. • They may contribute to black hole growth over c ...
... Why Search For Tidal Disruption Events? • They are an unambiguous probe for supermassive black holes lurking in the nuclei of normal galaxies. • The luminosity, temperature, and decay of the flare is dependent on the mass and spin of the black hole. • They may contribute to black hole growth over c ...
Dark Matter NS Warsaw
... ▸ Since the dark matter density near the Galactic center is significantly higher than regions near the solar position (where the oldest pulsars have been found) there is a parameter space where dark matter accumulation may solve the missing pulsar problem. ...
... ▸ Since the dark matter density near the Galactic center is significantly higher than regions near the solar position (where the oldest pulsars have been found) there is a parameter space where dark matter accumulation may solve the missing pulsar problem. ...
Effects of triple-α and C(α, γ )16 O reaction rates on the supernova
... The triple-α and 12 C(α, γ )16 O rates are the key nuclear reaction rates concerning He-burning in massive star evolution. As a consequence, explosive nucleosynthesis and the resulting supernova yields of a massive star would be influenced seriously by the two rates. We select four combinations from ...
... The triple-α and 12 C(α, γ )16 O rates are the key nuclear reaction rates concerning He-burning in massive star evolution. As a consequence, explosive nucleosynthesis and the resulting supernova yields of a massive star would be influenced seriously by the two rates. We select four combinations from ...
CBP's Powerpoint template for scientific posters
... objects (nearly all LBLs) defined by Kühr & Schmidt (1990) were obtained at 5, 8.4 and 15 GHz in February 1997, April 1997 or June 1999. These data were calibrated and imaged in the NRAO AIPS package following standard techniques; previous rotation-measure results for several individual sources are ...
... objects (nearly all LBLs) defined by Kühr & Schmidt (1990) were obtained at 5, 8.4 and 15 GHz in February 1997, April 1997 or June 1999. These data were calibrated and imaged in the NRAO AIPS package following standard techniques; previous rotation-measure results for several individual sources are ...
Star Magnitude - ScienceEducationatNewPaltz
... larger than 6 ( 6, 7, 8, 9, ... 30th ... etc.) The Hubble Space Telescope Deep Field image contains some galaxies as faint as 30th magnitude. First magnitude stars are corrected across the scale of 1, 0, -1 with the brightest star Sirius at -1.44. The scale increases in brightness with negative numb ...
... larger than 6 ( 6, 7, 8, 9, ... 30th ... etc.) The Hubble Space Telescope Deep Field image contains some galaxies as faint as 30th magnitude. First magnitude stars are corrected across the scale of 1, 0, -1 with the brightest star Sirius at -1.44. The scale increases in brightness with negative numb ...
Investigating the Spectral Energy Distribution TARA JILL PARKIN
... In particular, the present-day structure of the ISM of a galaxy is strongly dependent on the evolution of its star formation rate (SFR). Clues as to previous episodes of star formation rates can be found in the various stellar populations within the galaxy (Tielens, 1995). Low-mass stars with long l ...
... In particular, the present-day structure of the ISM of a galaxy is strongly dependent on the evolution of its star formation rate (SFR). Clues as to previous episodes of star formation rates can be found in the various stellar populations within the galaxy (Tielens, 1995). Low-mass stars with long l ...
01_test_bank
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) Our view of distant objects is obscured by gas and dust when we look into the galactic plane. D) The galaxy is about 100,000 light-years in diameter. E) One ro ...
... A) It contains between 100 billion and 1 trillion stars. B) Our solar system is located very close to the center of the Milky Way Galaxy. C) Our view of distant objects is obscured by gas and dust when we look into the galactic plane. D) The galaxy is about 100,000 light-years in diameter. E) One ro ...
Learning Objectives - UNC Physics and Astronomy
... Curtis argued that the solar system is near or at the center of the Milky Way galaxy, and that the Milky Way is about 10 kpc across. Shapley, on the other hand, argued that the solar system is in the outskirts of the Milky Way, and that the Milky Way is about 100 kpc across. In section A of the proc ...
... Curtis argued that the solar system is near or at the center of the Milky Way galaxy, and that the Milky Way is about 10 kpc across. Shapley, on the other hand, argued that the solar system is in the outskirts of the Milky Way, and that the Milky Way is about 100 kpc across. In section A of the proc ...
A Collection of Curricula for the STARLAB Polynesian Voyaging
... familiar to the Hawaiians. They may not have understood that the nightly movement was due to the rotation of the earth on its axis and the yearly movement to its revolution around the Sun, but they made good use of these movements and could measure the time of night and the calendar of events with c ...
... familiar to the Hawaiians. They may not have understood that the nightly movement was due to the rotation of the earth on its axis and the yearly movement to its revolution around the Sun, but they made good use of these movements and could measure the time of night and the calendar of events with c ...
Spectral Fingerprints of Earth-like Planets Around FGK Stars
... from the VIS to IR (0.4 to 20 lm) to compare detectability of features in different wavelength ranges in accordance with the James Webb Space Telescope and future design concepts to characterize exo-Earths. We have also explored the effect of the stellar UV levels as well as spectral energy distribu ...
... from the VIS to IR (0.4 to 20 lm) to compare detectability of features in different wavelength ranges in accordance with the James Webb Space Telescope and future design concepts to characterize exo-Earths. We have also explored the effect of the stellar UV levels as well as spectral energy distribu ...
Testing the evolution of the DB white dwarf GD 358: first results of a
... independent pulsations periods of GD 358 is done using the GA optimization method developed by M0 and M1. This method improves the objective search in the parameter space over traditional procedures like iterative methods starting from a first guess. This standard approach has a potential problem: t ...
... independent pulsations periods of GD 358 is done using the GA optimization method developed by M0 and M1. This method improves the objective search in the parameter space over traditional procedures like iterative methods starting from a first guess. This standard approach has a potential problem: t ...
ASTR 31: Descriptive Astronomy
... beryllium-8 (4 protons + 4 neutrons): 8Be carbon-12 (6 protons + 6 neutrons): 12C oxygen-16 (8 protons + 8 neutrons): 16O neon-20 (10 protons + 10 neutrons): 20Ne magnesium-24 (12 protons + 12 neutrons): 24Mg silicon-28 (14 protons + 14 neutrons): 28Si sulfer-32 (16 protons + 16 neutrons): 32S argon ...
... beryllium-8 (4 protons + 4 neutrons): 8Be carbon-12 (6 protons + 6 neutrons): 12C oxygen-16 (8 protons + 8 neutrons): 16O neon-20 (10 protons + 10 neutrons): 20Ne magnesium-24 (12 protons + 12 neutrons): 24Mg silicon-28 (14 protons + 14 neutrons): 28Si sulfer-32 (16 protons + 16 neutrons): 32S argon ...
test - Scioly.org
... including what types of stars generally use one or the other. (8 points) 6) A star with low to medium mass (0.5 - 8 solar masses) will not be hot enough to fuse ___________ into ____________, so it will have a __________________________ core. 7) Given that a certain star lacks a corona and has a con ...
... including what types of stars generally use one or the other. (8 points) 6) A star with low to medium mass (0.5 - 8 solar masses) will not be hot enough to fuse ___________ into ____________, so it will have a __________________________ core. 7) Given that a certain star lacks a corona and has a con ...
A radio-pulsing white dwarf binary star
... White dwarfs are not born spinning rapidly24 , and a prior stage of accretion-driven spin-up is required. Depending upon the distance at which the accreting material coupled to the white dwarf’s magnetic field, between 0.002 M and 0.015 M of matter are required to reach PS = 1.95 min. For an accre ...
... White dwarfs are not born spinning rapidly24 , and a prior stage of accretion-driven spin-up is required. Depending upon the distance at which the accreting material coupled to the white dwarf’s magnetic field, between 0.002 M and 0.015 M of matter are required to reach PS = 1.95 min. For an accre ...
A Star*s Color, Temperature, and Brightness are Related!
... • What is the peak wavelength of our sun, with a T = 5778 K? 2.9 x 106 = 502 nm (yellowish-green) 5778 K • What is the peak wavelength of a star with a surface temperature of 3500 K? 2.9 x 106 = 829 nm (this star emits the 3500 K majority of its light as infrared, IR). ...
... • What is the peak wavelength of our sun, with a T = 5778 K? 2.9 x 106 = 502 nm (yellowish-green) 5778 K • What is the peak wavelength of a star with a surface temperature of 3500 K? 2.9 x 106 = 829 nm (this star emits the 3500 K majority of its light as infrared, IR). ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... [Fe/H]≤ −4.5 are CEMP-no stars. These objects have peculiar chemical abundance patterns consistent with the yields predicted for primordial faint SN (e.g. Iwamoto et al. 2005). However, we also note that these extreme stars are part of a common, global trend, which involves stars in both the Galacti ...
... [Fe/H]≤ −4.5 are CEMP-no stars. These objects have peculiar chemical abundance patterns consistent with the yields predicted for primordial faint SN (e.g. Iwamoto et al. 2005). However, we also note that these extreme stars are part of a common, global trend, which involves stars in both the Galacti ...
Distance determination for RAVE stars using stellar models
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
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.