Lecture Slides – Stars
... Planetary Nebula (lifetime ca. 10,000 years, from expansion) + remnant carbon-oxygen white dwarf (electron degenerate) ...
... Planetary Nebula (lifetime ca. 10,000 years, from expansion) + remnant carbon-oxygen white dwarf (electron degenerate) ...
Slide 1
... Spectral Lines … Bottom Line Kirchhoff’s laws: 1. Luminous solid, liquid, or dense gas produces continuous spectrum 2. Low-density hot gas produces emission spectrum 3. Continuous spectrum incident on cool, thin gas produces absorption spectrum ...
... Spectral Lines … Bottom Line Kirchhoff’s laws: 1. Luminous solid, liquid, or dense gas produces continuous spectrum 2. Low-density hot gas produces emission spectrum 3. Continuous spectrum incident on cool, thin gas produces absorption spectrum ...
The star Betelgeuse is about 500 light years away from us. If this star
... a) Procyon is moving at the same speed as Acrux b) Procyon is moving more slowly than Acrux c) Procyon and Acrux are BOTH moving away from the Sun d) both b & c e) none of the above Which of the following is NOT an implication of Hubble's law? a) the Universe is expanding b) we are at the center of ...
... a) Procyon is moving at the same speed as Acrux b) Procyon is moving more slowly than Acrux c) Procyon and Acrux are BOTH moving away from the Sun d) both b & c e) none of the above Which of the following is NOT an implication of Hubble's law? a) the Universe is expanding b) we are at the center of ...
The difficulty of forming large disk galaxies with small bulges
... cooled (or heated) so that the OVI is undetectable The gaseous halo may be a basic component of star forming galaxies that is removed or transformed when star formation is quenched. cf the Fraternali & Binney 2008 mechanism of halo gas entrainment: star formation drives the entrainment which then fe ...
... cooled (or heated) so that the OVI is undetectable The gaseous halo may be a basic component of star forming galaxies that is removed or transformed when star formation is quenched. cf the Fraternali & Binney 2008 mechanism of halo gas entrainment: star formation drives the entrainment which then fe ...
Li-cai Deng
... that order, as available. A u-band survey is planned on the 2.3 meter Bok telescope of Arizona’s Steward Observatory; a camera is currently being fabricated. This survey can be used in conjunction with PanSTARRS or SuperCOSMOS (1) Select as many 0.1<(g-r)0<1.0, g0<17 stars as possible (a nearly comp ...
... that order, as available. A u-band survey is planned on the 2.3 meter Bok telescope of Arizona’s Steward Observatory; a camera is currently being fabricated. This survey can be used in conjunction with PanSTARRS or SuperCOSMOS (1) Select as many 0.1<(g-r)0<1.0, g0<17 stars as possible (a nearly comp ...
Name - CLC Charter School
... When the supernova is done exploding, as an effect of the large transfer of matter and energy, there is a very different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can l ...
... When the supernova is done exploding, as an effect of the large transfer of matter and energy, there is a very different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can l ...
Origin of the Solar System
... At low pressures, such as those found in space, cooling materials generally condense directly from a gas into a solid. • When the solar system formed, temperatures near the ...
... At low pressures, such as those found in space, cooling materials generally condense directly from a gas into a solid. • When the solar system formed, temperatures near the ...
Spying into the lives of the stars
... stations, having them fill out an attached worksheet for each station. Lesson Closure: After students have completed all of the stations, have them share their Haikus with the class. Use this as an entry into a discussion of stellar evolution using the stars from the H-R diagram. Ask them, which of ...
... stations, having them fill out an attached worksheet for each station. Lesson Closure: After students have completed all of the stations, have them share their Haikus with the class. Use this as an entry into a discussion of stellar evolution using the stars from the H-R diagram. Ask them, which of ...
The local ISM in three dimensions: kinematics
... nearby warm partially ionized interstellar gas including the identification of structures, which we call clouds, measurement of their kinematic and physical properties, characterization of the ionized gas surrounding the clouds, and, when feasible, identification of the physical processes responsibl ...
... nearby warm partially ionized interstellar gas including the identification of structures, which we call clouds, measurement of their kinematic and physical properties, characterization of the ionized gas surrounding the clouds, and, when feasible, identification of the physical processes responsibl ...
The Milky Way Galaxy
... Which of the following is NOT a good reason for learning more about dark matter? dark matter provides the gravitational force that holds galaxies together the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter ...
... Which of the following is NOT a good reason for learning more about dark matter? dark matter provides the gravitational force that holds galaxies together the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter ...
A Question of Planets - Vanderbilt University
... around three classical T Tauri stars with visible protoplanetary disks. They have found that the strength of the hydrogen emission lines in the three is comparable to that measured at DoAr21.They have used these results to obtain the ratio between the mass of hydrogen molecules that are producing th ...
... around three classical T Tauri stars with visible protoplanetary disks. They have found that the strength of the hydrogen emission lines in the three is comparable to that measured at DoAr21.They have used these results to obtain the ratio between the mass of hydrogen molecules that are producing th ...
in search of antimatter in the universe
... may include the jets of Active Galactic Nuclei (AGN) (See title, Figure 4,5) These colossal jets originate from the central super-massive black hole of the galaxy, flying through the galaxy around them at speeds close to the speed of light. It is possible that these jets contain electrons and positr ...
... may include the jets of Active Galactic Nuclei (AGN) (See title, Figure 4,5) These colossal jets originate from the central super-massive black hole of the galaxy, flying through the galaxy around them at speeds close to the speed of light. It is possible that these jets contain electrons and positr ...
Disk Instability Models
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
Who’s Afraid of a Stellar Superflare? Rachel Osten GSFC
... in solar flares, produced by fluorescence off cold iron in photosphere; probe of both photospheric abundance and height of irradiating structure (e.g. Bai 1979) possibly also collisional ionization (Emslie et al. 1986) Osten et al. (2007) favored collisional interpretation due to reaching Compton sc ...
... in solar flares, produced by fluorescence off cold iron in photosphere; probe of both photospheric abundance and height of irradiating structure (e.g. Bai 1979) possibly also collisional ionization (Emslie et al. 1986) Osten et al. (2007) favored collisional interpretation due to reaching Compton sc ...
The star formation histories of two northern LMC fields
... The star formation histories of two northern LMC fields (1993) UBV charge-coupled devices (CCD) photometry near the NGC 2004 field and the Lucke (1972) BV photoelectric photometry of LH 77 (two of the Constellation III fields). Our values were consistent with the Balona & Jerzykiewicz (1993) result ...
... The star formation histories of two northern LMC fields (1993) UBV charge-coupled devices (CCD) photometry near the NGC 2004 field and the Lucke (1972) BV photoelectric photometry of LH 77 (two of the Constellation III fields). Our values were consistent with the Balona & Jerzykiewicz (1993) result ...
December
... A T-shaped asterism just east of gamma Oph; it is formed by the stars 66 Oph, 67 Oph, 68 Oph and 70 Oph “The Arrow” is a little over 3 degrees east of Beta Ophiuchi . Below “The Arrow” is Barnard’s Star. It shines dimly at magnitude 9.5. Discovered by E. E. Barnard in 1916, it is a red dwarf located ...
... A T-shaped asterism just east of gamma Oph; it is formed by the stars 66 Oph, 67 Oph, 68 Oph and 70 Oph “The Arrow” is a little over 3 degrees east of Beta Ophiuchi . Below “The Arrow” is Barnard’s Star. It shines dimly at magnitude 9.5. Discovered by E. E. Barnard in 1916, it is a red dwarf located ...
A0620-00 poster
... As the brightest dwarf nova and one of the brightest cataclysmic variables of any kind, SS Cygni has been extensively observed. Its outbursts, for example, have been continuously monitored since 1896 and their properties are the gold standard against which accretion disk instability models for dwarf ...
... As the brightest dwarf nova and one of the brightest cataclysmic variables of any kind, SS Cygni has been extensively observed. Its outbursts, for example, have been continuously monitored since 1896 and their properties are the gold standard against which accretion disk instability models for dwarf ...
A Universe of Galaxies - Pennsylvania State University
... do not produce much radio emission). They were named quasistellar radio sources (quasars, or QSOs): ...
... do not produce much radio emission). They were named quasistellar radio sources (quasars, or QSOs): ...
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.