![here - SDSU Astronomy Department and Mount Laguna Observatory](http://s1.studyres.com/store/data/008080216_1-88ca598ef62779c40b07421db5578f8b-300x300.png)
here - SDSU Astronomy Department and Mount Laguna Observatory
... In many cases, this is because they are pulsating. The radius and temperature changes over the cycle, giving rise to brightness variations. Image from Nick Strobel’s Astronomy Notes (http://www.astronomynotes.com) ...
... In many cases, this is because they are pulsating. The radius and temperature changes over the cycle, giving rise to brightness variations. Image from Nick Strobel’s Astronomy Notes (http://www.astronomynotes.com) ...
NAME
... 1. What did Edwin Hubble study in the Andromeda Galaxy that proved it was an individual galaxy and not part of our own Milky Way? a. Cepheid stars b. Type I supernovae c. globular clusters d. red giant stars e. RR Lyrae variables ...
... 1. What did Edwin Hubble study in the Andromeda Galaxy that proved it was an individual galaxy and not part of our own Milky Way? a. Cepheid stars b. Type I supernovae c. globular clusters d. red giant stars e. RR Lyrae variables ...
Cooling of Compact Stars
... The Astrophysical Journal V 749 N1 Chris L. Fryer et al. 2012 ApJ 749 91 ...
... The Astrophysical Journal V 749 N1 Chris L. Fryer et al. 2012 ApJ 749 91 ...
presentation
... O-rich photosphere C-rich photosphere “Carbon stars” (C2, CN, HCN, C2H2 features in optical/IR spectra) s-process elements (Ba, La, Eu, Tc, etc) 3. Enrichment of ISM via mass loss Major “Dust Factory”, together with supernovae ...
... O-rich photosphere C-rich photosphere “Carbon stars” (C2, CN, HCN, C2H2 features in optical/IR spectra) s-process elements (Ba, La, Eu, Tc, etc) 3. Enrichment of ISM via mass loss Major “Dust Factory”, together with supernovae ...
Stellar Relaxation Times
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
NO GAP BUT LOCAL MINIMA
... This result only includes NaCo-LP targets: we will include archival data as well. We will explore different combinations of β1 and outer truncation radius. (Reggiani et al., in preparation) ...
... This result only includes NaCo-LP targets: we will include archival data as well. We will explore different combinations of β1 and outer truncation radius. (Reggiani et al., in preparation) ...
The origin of elements For life we need some complexity, and
... In contrast to the quick production of hydrogen and helium in just the first few minutes of the universe, other elements take a long time indeed. Stars are powered by nuclear fusion, in which light nuclei combine to make heavier nuclei. For most of their life, on the so-called “main sequence”, stars ...
... In contrast to the quick production of hydrogen and helium in just the first few minutes of the universe, other elements take a long time indeed. Stars are powered by nuclear fusion, in which light nuclei combine to make heavier nuclei. For most of their life, on the so-called “main sequence”, stars ...
What keeps stars shining? What holds them up? Lecture 14. The
... • Why does the main sequence luminosity increase so rapidly with mass? The central temperature of more massive stars must be higher to support additional material. The Hydrogen fusion rate is very sensitive to the star's central temperature. • Main sequence stars are especially stable because of the ...
... • Why does the main sequence luminosity increase so rapidly with mass? The central temperature of more massive stars must be higher to support additional material. The Hydrogen fusion rate is very sensitive to the star's central temperature. • Main sequence stars are especially stable because of the ...
History of Star Formation in Local Galaxies
... Full analysis of the CMDs is not complete yet, but simply from comparing the CMDs to isochrones, we find that the SMC does have 10-12 Gyr old stars. Just not that many. Thus the SMC had a slow start to its formation… which maybe a reason so few globular clusters formed in it. ...
... Full analysis of the CMDs is not complete yet, but simply from comparing the CMDs to isochrones, we find that the SMC does have 10-12 Gyr old stars. Just not that many. Thus the SMC had a slow start to its formation… which maybe a reason so few globular clusters formed in it. ...
Planetary Companions to Evolved Intermediate
... of A dwarfs sufficient for the detection of substellar companions). This is actually one of the major reasons why targets for planet searches had been limited to low-mass (< 1.5Mˇ ) F–M dwarfs. On the contrary, late G to early K giants and subgiants, which are intermediate-mass stars in evolved stag ...
... of A dwarfs sufficient for the detection of substellar companions). This is actually one of the major reasons why targets for planet searches had been limited to low-mass (< 1.5Mˇ ) F–M dwarfs. On the contrary, late G to early K giants and subgiants, which are intermediate-mass stars in evolved stag ...
Lecture5
... When one star of a binary gets behind the other star, eclipse happens. The intensity (brightness) of the binary vs time curve is called `light curve’. Then the shape of the light curve can often determine various useful parameters, e.g., the inclination angle , nature of the stellar atmosphere, and ...
... When one star of a binary gets behind the other star, eclipse happens. The intensity (brightness) of the binary vs time curve is called `light curve’. Then the shape of the light curve can often determine various useful parameters, e.g., the inclination angle , nature of the stellar atmosphere, and ...
The Chemical Composition of the Local Interstellar Dust
... abundance reference: Sun, local F & G stars, B stars Sun: + star that can be studied best + independent abundances from different indicators - 4.56 Gyr old, representative for present-day ISM? F&G stars: + differential abundances relative to Sun + increased number statistics - difficult age determin ...
... abundance reference: Sun, local F & G stars, B stars Sun: + star that can be studied best + independent abundances from different indicators - 4.56 Gyr old, representative for present-day ISM? F&G stars: + differential abundances relative to Sun + increased number statistics - difficult age determin ...
network of amateur astronomers (CBA) to gather data on CV`s.
... c. May be updated daily. 2. Astrometric Catalogs a. Magnitudes listed in the astrometric catalog (with the possible exception of CMC 14 red magnitudes) are notoriously bad. b. USNO-A2.0 contains entries for over a half billion stars. Obsolete because it doesn’t contain proper motions. c. USNO-B1.0 c ...
... c. May be updated daily. 2. Astrometric Catalogs a. Magnitudes listed in the astrometric catalog (with the possible exception of CMC 14 red magnitudes) are notoriously bad. b. USNO-A2.0 contains entries for over a half billion stars. Obsolete because it doesn’t contain proper motions. c. USNO-B1.0 c ...
Astronomy C - Scioly.org
... 59. What is the term for a gas giant that has had its atmosphere stripped away? 60. How are ocean planets thought to form? 61. What is one possibility for why a planet may be orbiting in the opposite direction to the rotation of its parent star? 62. What are the two main reasons for why we preferent ...
... 59. What is the term for a gas giant that has had its atmosphere stripped away? 60. How are ocean planets thought to form? 61. What is one possibility for why a planet may be orbiting in the opposite direction to the rotation of its parent star? 62. What are the two main reasons for why we preferent ...
Stability of hot neutron stars
... It is likely that matter in a neutron star crust is compressed by accreting matter and/or by the slowingdown of its rotation after the freezing of thermonuclear equilibrium. The change of nuclear compositions, which takes place during the compression, has been investigated. If the initial species of ...
... It is likely that matter in a neutron star crust is compressed by accreting matter and/or by the slowingdown of its rotation after the freezing of thermonuclear equilibrium. The change of nuclear compositions, which takes place during the compression, has been investigated. If the initial species of ...
The First Stars in the Universe - Scientific American
... models predict that these clumps would gradually evolve into gravitationally bound structures. Smaller systems would form first and then merge into larger agglomerations. The denser regions would take the form of a network of filaments, and the first star-forming systems—small protogalaxies—would co ...
... models predict that these clumps would gradually evolve into gravitationally bound structures. Smaller systems would form first and then merge into larger agglomerations. The denser regions would take the form of a network of filaments, and the first star-forming systems—small protogalaxies—would co ...
WASP-86b and WASP-102b: super-dense versus bloated planets
... just to mention a few, are capable of detecting peculiar objects for example HATS-17 b, (Penev et al. 2016); HATS-18 b, (Brahm et al. 2016), increasing the spectrum of possible massradius relations in the planetary regime. These systems provide invaluable observational constraints on theoretical mod ...
... just to mention a few, are capable of detecting peculiar objects for example HATS-17 b, (Penev et al. 2016); HATS-18 b, (Brahm et al. 2016), increasing the spectrum of possible massradius relations in the planetary regime. These systems provide invaluable observational constraints on theoretical mod ...
Galaxies - sciencejedi.com
... that the total mass is on order of 100 trillion solar masses (1012 M⊙ ). • In 2005, it was discovered that the Milky Way does not have a spherical bulge, but rather an elongated bar structure in the core. The bar was difficult to observe due to obscuration by dust and gas, but also because we are lo ...
... that the total mass is on order of 100 trillion solar masses (1012 M⊙ ). • In 2005, it was discovered that the Milky Way does not have a spherical bulge, but rather an elongated bar structure in the core. The bar was difficult to observe due to obscuration by dust and gas, but also because we are lo ...
The Big Bang Is Bunk - 21stcenturysciencetech.com
... and are independent of distance from the observer. The Doppler phenomenon has been used since the last quarter of the 19th century to study double stars, motions of the Sun, and rotation of celestial objects. There are always equal and opposite redshifts and blueshifts separated by null. The shifts ...
... and are independent of distance from the observer. The Doppler phenomenon has been used since the last quarter of the 19th century to study double stars, motions of the Sun, and rotation of celestial objects. There are always equal and opposite redshifts and blueshifts separated by null. The shifts ...
Where Do Baby Stars Come From?
... When you look at them, you can look at the elements within them and say, “this had a supernova that contributed to it, this one had two or three.” This is the result of two different types of research. You have people who say, “okay, when you have a supernova explosion from a massive star that is te ...
... When you look at them, you can look at the elements within them and say, “this had a supernova that contributed to it, this one had two or three.” This is the result of two different types of research. You have people who say, “okay, when you have a supernova explosion from a massive star that is te ...
Winter Night Sky Guide
... 12. Moving to Orion’s right knee, you will see a bright, bluish star. This is Rigel and it is another type of supergiant, a blue supergiant naturally. Betelgeuse would have looked something like this before it started to run short on fuel. Like Betelgeuse, Rigel is much more massive than our Sun but ...
... 12. Moving to Orion’s right knee, you will see a bright, bluish star. This is Rigel and it is another type of supergiant, a blue supergiant naturally. Betelgeuse would have looked something like this before it started to run short on fuel. Like Betelgeuse, Rigel is much more massive than our Sun but ...
GALEX UV Light-curves of M-Dwarf Flare Stars: THE FLARING UV
... - a rapid rise in flux followed by a gradual decay - a rapid rise in flux followed by further, sometimes larger, eruptions with long decay times ...
... - a rapid rise in flux followed by a gradual decay - a rapid rise in flux followed by further, sometimes larger, eruptions with long decay times ...
A Catalog of Blue Stragglers in Open Clusters
... Quality of the color-magnitude and color-color diagrams ...
... Quality of the color-magnitude and color-color diagrams ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.