The Cosmic Perspective Our Galaxy
... What causes the blue and red colors in a photograph of a typical nebula? a) The ionizing photons from a hot star cause hydrogen gas to glow red and helium to glow blue. b) Dust grains scatter blue light and let red light pass through, similar to the blue sky and red sunsets in our atmosphere. c) ...
... What causes the blue and red colors in a photograph of a typical nebula? a) The ionizing photons from a hot star cause hydrogen gas to glow red and helium to glow blue. b) Dust grains scatter blue light and let red light pass through, similar to the blue sky and red sunsets in our atmosphere. c) ...
shirley - Yancy L. Shirley`s Webpage
... SF in Dense Cores Star formation occurs within dense molecular cores High density gas in dense cores (n > 106 cm-3) Clumpy/filamentary structures within molecular cloud ...
... SF in Dense Cores Star formation occurs within dense molecular cores High density gas in dense cores (n > 106 cm-3) Clumpy/filamentary structures within molecular cloud ...
Magnetic cycles of Sun-like stars with different levels of coronal and
... Figures 1,2 show that the more sun-like stars in pattern, the greater the spread in their luminosities MV and chromospheric activity CA versus the Sun value. It is important to note that the study of CA of stars are performed for very large data sets. Zhao et al. 2015 have studied a sample of ∼ 120 ...
... Figures 1,2 show that the more sun-like stars in pattern, the greater the spread in their luminosities MV and chromospheric activity CA versus the Sun value. It is important to note that the study of CA of stars are performed for very large data sets. Zhao et al. 2015 have studied a sample of ∼ 120 ...
Document
... Jet (~ continuous flow of emission) close to source Knots with “empty space” further out Only in the past 10 years that we have Realised that outflows can extend for many parsecs 1pc ~ 3 X 1013 km ~ 3.26 light years ~ 206265 AU Can outflows be larger than their parent cloud? ...
... Jet (~ continuous flow of emission) close to source Knots with “empty space” further out Only in the past 10 years that we have Realised that outflows can extend for many parsecs 1pc ~ 3 X 1013 km ~ 3.26 light years ~ 206265 AU Can outflows be larger than their parent cloud? ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
@let@token Stellar Oscillations: Pulsations of Stars Throughout the
... vection zone deepens, and lower frequency modes become overstable. However, the deeper convection zone impedes the passage of Ñux perturbations from the base of the convection zone to the photosphere. Thus the photometric variation of a mode with constant velocity amplitude decreases. These factors ...
... vection zone deepens, and lower frequency modes become overstable. However, the deeper convection zone impedes the passage of Ñux perturbations from the base of the convection zone to the photosphere. Thus the photometric variation of a mode with constant velocity amplitude decreases. These factors ...
Spectroscopic Variability of Supergiant Star HD14134, B3Ia
... typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were processed separately. These data are presented in Fi ...
... typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were processed separately. These data are presented in Fi ...
Spectroscopic Variability of Supergiant Star HD14134, B3Ia
... typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were processed separately. These data are presented in Fi ...
... typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were processed separately. These data are presented in Fi ...
Primas
... Log g and metallicity sensiDvity is low, some dependence on the mixing-‐length parameter (Hβ and higher). ...
... Log g and metallicity sensiDvity is low, some dependence on the mixing-‐length parameter (Hβ and higher). ...
offprint - UW-Madison Astronomy - University of Wisconsin–Madison
... of Rasalhague motivating future detailed asteroseismic modeling—a source with a precisely measured parallax distance, photospheric oblateness, latitude temperature structure, and whose low-mass companion provides an astrometric orbit for precise mass determinations. Key words: binaries: close – star ...
... of Rasalhague motivating future detailed asteroseismic modeling—a source with a precisely measured parallax distance, photospheric oblateness, latitude temperature structure, and whose low-mass companion provides an astrometric orbit for precise mass determinations. Key words: binaries: close – star ...
Test - Scioly.org
... D. Secondary Minimum E. Orbital Secondary 56. If the entire X-Axis (as strictly measured on the graph) spans 1.641 units, calculate the approximate period and frequency of the described binary system. A. Period: .876; Frequency: 1.14 B. Period: .853; Frequency: 1.17 C. Period: .821; Frequency: 1.21 ...
... D. Secondary Minimum E. Orbital Secondary 56. If the entire X-Axis (as strictly measured on the graph) spans 1.641 units, calculate the approximate period and frequency of the described binary system. A. Period: .876; Frequency: 1.14 B. Period: .853; Frequency: 1.17 C. Period: .821; Frequency: 1.21 ...
Lab 7
... Introduction: By looking at an apparently flat background of stars at night or at a star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of ...
... Introduction: By looking at an apparently flat background of stars at night or at a star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of ...
PARALLAX, THE LAB
... to be covering. With that observation made and recorded, the finger person will close that eye, open the other eye and determine what area the finger covers in that situation. The shift in apparent covering will be designated “s” (see sketch). Along with that information, you will also need to know ...
... to be covering. With that observation made and recorded, the finger person will close that eye, open the other eye and determine what area the finger covers in that situation. The shift in apparent covering will be designated “s” (see sketch). Along with that information, you will also need to know ...
Introduction to Telescopes
... rotates) around the axis that connects the north and south celestial poles. At the latitude of Brown University, the pole star is at an altitude of approximately 41 degrees. Suppose that we would like our telescope to be able to track the motions of the stars as trace giant circles around the pole s ...
... rotates) around the axis that connects the north and south celestial poles. At the latitude of Brown University, the pole star is at an altitude of approximately 41 degrees. Suppose that we would like our telescope to be able to track the motions of the stars as trace giant circles around the pole s ...
Stellar Spectroscopy (GA 3.0) - National Optical Astronomy
... some stars, emission lines as well. These spectral lines can be used to determine an incredible amount of information about the star, including its temperature, composition, size, velocity and age, as well as many other properties. Most of what we know about stars has been determined by the study of ...
... some stars, emission lines as well. These spectral lines can be used to determine an incredible amount of information about the star, including its temperature, composition, size, velocity and age, as well as many other properties. Most of what we know about stars has been determined by the study of ...
Larger, high-res file, best for printing
... when Cassiopeia was high in the daylight sky. Or this particular supernova may have had such a low intrinsic luminosity that it was simply too dim for most 17th-century astronomers to notice. Alternatively, the Cas A event may have been a typical luminous supernova that was heavily obscured by inter ...
... when Cassiopeia was high in the daylight sky. Or this particular supernova may have had such a low intrinsic luminosity that it was simply too dim for most 17th-century astronomers to notice. Alternatively, the Cas A event may have been a typical luminous supernova that was heavily obscured by inter ...
Spiral structure of the Third Galactic Quadrant and the solution to the
... galaxy 1-2 Gyr ago (which, given that it is a 1-2 Gyr population, should also have a red clump). This piece of evidence has been taken to be an unambiguous indicator of the reality of CMa given that it does not correspond to any known Galactic component. Additionally, the narrowness of the BP, which ...
... galaxy 1-2 Gyr ago (which, given that it is a 1-2 Gyr population, should also have a red clump). This piece of evidence has been taken to be an unambiguous indicator of the reality of CMa given that it does not correspond to any known Galactic component. Additionally, the narrowness of the BP, which ...
Hipparcos
Hipparcos was a scientific satellite of the European Space Agency (ESA), launched in 1989 and operated until 1993. It was the first space experiment devoted to precision astrometry, the accurate measurement of the positions of celestial objects on the sky. This permitted the accurate determination of proper motions and parallaxes of stars, allowing a determination of their distance and tangential velocity. When combined with radial-velocity measurements from spectroscopy, this pinpointed all six quantities needed to determine the motion of stars. The resulting Hipparcos Catalogue, a high-precision catalogue of more than 118,200 stars, was published in 1997. The lower-precision Tycho Catalogue of more than a million stars was published at the same time, while the enhanced Tycho-2 Catalogue of 2.5 million stars was published in 2000. Hipparcos ' follow-up mission, Gaia, was launched in 2013.The word ""Hipparcos"" is an acronym for High precision parallax collecting satellite and also a reference to the ancient Greek astronomer Hipparchus of Nicaea, who is noted for applications of trigonometry to astronomy and his discovery of the precession of the equinoxes.