Astronomy 16: Introduction
... - in binary systems, some lines do not show Doppler shift due to binary motion Astronomy 16: The Interstellar Medium ...
... - in binary systems, some lines do not show Doppler shift due to binary motion Astronomy 16: The Interstellar Medium ...
Lecture 14
... satellites into space to measure very precise parallax? • Would it be easier to measure parallax from Jupiter? From Venus? ...
... satellites into space to measure very precise parallax? • Would it be easier to measure parallax from Jupiter? From Venus? ...
The Circumstellar Medium of Massive Stars in Motion
... 0.5 × 1020 cm−2 ). We found that the H II region generates a dense expanding shell expanding from its lateral surfaces, leaving a conical shell (with a large momentum) enclosing an underdense wake trailing behind it. This shell should be observable in neutral hydrogen emission at 21 cm, although its ...
... 0.5 × 1020 cm−2 ). We found that the H II region generates a dense expanding shell expanding from its lateral surfaces, leaving a conical shell (with a large momentum) enclosing an underdense wake trailing behind it. This shell should be observable in neutral hydrogen emission at 21 cm, although its ...
– 1 – 1. Galaxy Observations 1.1.
... rate affecting the UV continuum, and the calibration for UV stellar photospheric features or UV ISM absorption to metallicity is not well understood at present (see Erb 2010 for details). So the best approach is to move into the near-IR, where the normal optical low redshift techniques and calibrati ...
... rate affecting the UV continuum, and the calibration for UV stellar photospheric features or UV ISM absorption to metallicity is not well understood at present (see Erb 2010 for details). So the best approach is to move into the near-IR, where the normal optical low redshift techniques and calibrati ...
A very massive runaway star from Cygnus OB2⋆
... v∗ is the spatial velocity of the star. The distance given in Eq. (5) assumes that the bow shock is bound by shock fronts on both sides. In reality, the non-zero cooling time of the shocked stellar wind builds up a thick layer of low-density, high-temperature gas between the reverse shock on the ste ...
... v∗ is the spatial velocity of the star. The distance given in Eq. (5) assumes that the bow shock is bound by shock fronts on both sides. In reality, the non-zero cooling time of the shocked stellar wind builds up a thick layer of low-density, high-temperature gas between the reverse shock on the ste ...
Comprehensive Census and Complete Characterization of Nearby
... Though there have been hundreds of debris disk stars published in the literature including those from WISE data searches (i.e. Wu et al. 2013, Patel et al. 2014), only a small fraction of those objects have comprehensive stellar and disk information necessary for uniting theories of planetary format ...
... Though there have been hundreds of debris disk stars published in the literature including those from WISE data searches (i.e. Wu et al. 2013, Patel et al. 2014), only a small fraction of those objects have comprehensive stellar and disk information necessary for uniting theories of planetary format ...
mufon ufo symposium -1974
... F5V to F7V have more stars rotating slowly indicating the possibility of planets. From approximately F8 on, all main sequence stars are rotating slowly, probably indicating planets. According to Carl Sagan, F8 is the point where intelligent life would have time to emerge. So main sequence stars fro ...
... F5V to F7V have more stars rotating slowly indicating the possibility of planets. From approximately F8 on, all main sequence stars are rotating slowly, probably indicating planets. According to Carl Sagan, F8 is the point where intelligent life would have time to emerge. So main sequence stars fro ...
Searching for the oldest, most metal-poor stars in the SkyMapper Survey
... capture by elements such as carbon and hence have atomic numbers that are multiples of four. Other fusion processes occured to create many additional elements. The large mass of these stars led them to expend their fuel faster and die earlier than smaller stars would. At the end of their lifetimes o ...
... capture by elements such as carbon and hence have atomic numbers that are multiples of four. Other fusion processes occured to create many additional elements. The large mass of these stars led them to expend their fuel faster and die earlier than smaller stars would. At the end of their lifetimes o ...
The Cosmic Perspective Our Galaxy
... • A supernova remnant cools and begins to emit visible light as it expands. • New elements made by a supernova mix into the interstellar medium. © 2014 Pearson Education, Inc. ...
... • A supernova remnant cools and begins to emit visible light as it expands. • New elements made by a supernova mix into the interstellar medium. © 2014 Pearson Education, Inc. ...
The Interstellar Medium White Paper
... gas has itself formed. But how do molecular clouds form in the first place? This fundamental process has yet to be observed. It is the rate-determining step for star formation itself. Observations of external spiral galaxies show that massive stars and their giant molecular clouds (GMCs) tend to for ...
... gas has itself formed. But how do molecular clouds form in the first place? This fundamental process has yet to be observed. It is the rate-determining step for star formation itself. Observations of external spiral galaxies show that massive stars and their giant molecular clouds (GMCs) tend to for ...
Chapter 17--Star Stuff
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
The star Epsilon UMa, or more commonly known as Alioth
... and the approximate surface temperature ranges from 7,500 to 11,000 degrees Kelvin. The average luminosity of these stars is around 80 solar luminosity (1 solar luminosity equaling 3.83 x 1033 ergs/s), the average mass is approximately 3.2 solar masses (1 solar mass equaling 1.989 x 1030 kg) and the ...
... and the approximate surface temperature ranges from 7,500 to 11,000 degrees Kelvin. The average luminosity of these stars is around 80 solar luminosity (1 solar luminosity equaling 3.83 x 1033 ergs/s), the average mass is approximately 3.2 solar masses (1 solar mass equaling 1.989 x 1030 kg) and the ...
Neutrinos and Nucleosynthesis
... and transition strengths, and the improvement of theoretical models and the possibility to run much more complex simulations. Today one knows that elements are produced in a process which is called nucleosynthesis. There are different types of nucleosynthesis. One type is the supernova nucleosynthes ...
... and transition strengths, and the improvement of theoretical models and the possibility to run much more complex simulations. Today one knows that elements are produced in a process which is called nucleosynthesis. There are different types of nucleosynthesis. One type is the supernova nucleosynthes ...
the solar neighborhood. xi. the trigonometric parallax of scr
... others are entirely new systems (e.g., Teegarden et al. 2003). The Research Consortium on Nearby Stars (RECONS) group seeks to identify and study all systems within 10 pc of the Sun. Previous papers of this series have used a variety of photometric and spectroscopic techniques to identify and study ...
... others are entirely new systems (e.g., Teegarden et al. 2003). The Research Consortium on Nearby Stars (RECONS) group seeks to identify and study all systems within 10 pc of the Sun. Previous papers of this series have used a variety of photometric and spectroscopic techniques to identify and study ...
Galaxy Spiral Arms
... Keplerian calculations are the absolute starting point, and then they find various ways, such as there being an extremely massive but invisible halo of dark matter surrounding the Galaxy, to explain the observed data. Since this is the case, essentially all Papers start off by assuming either of two ...
... Keplerian calculations are the absolute starting point, and then they find various ways, such as there being an extremely massive but invisible halo of dark matter surrounding the Galaxy, to explain the observed data. Since this is the case, essentially all Papers start off by assuming either of two ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... to expand the effective search volume. In PY 2010, PALFA continued processing data via the Einstein@Home community, which was originally developed to process LIGO data for coherent gravitational wave signals. E@H now devotes 1/3 of its processing resources to PALFA data to search for very compact bi ...
... to expand the effective search volume. In PY 2010, PALFA continued processing data via the Einstein@Home community, which was originally developed to process LIGO data for coherent gravitational wave signals. E@H now devotes 1/3 of its processing resources to PALFA data to search for very compact bi ...
Shortв•`lived radioactivity in the early solar system: The Superв•`AGB
... that is expected to develop a degenerate O–Ne core has approximately 5–9 Mx as lower limit and approximately 9–11 Mx as upper limit, also depending on the metallicity (see, e.g., Fig. 5 of Siess 2007). Given this high uncertainty it is not known how important the contribution of Super-AGB stars to t ...
... that is expected to develop a degenerate O–Ne core has approximately 5–9 Mx as lower limit and approximately 9–11 Mx as upper limit, also depending on the metallicity (see, e.g., Fig. 5 of Siess 2007). Given this high uncertainty it is not known how important the contribution of Super-AGB stars to t ...
Chapter 12: The Life Cycle of Stars
... What prevents protostars from continually collapsing ever smaller? If M > 0.08 MSun, then gravitational contraction heats the core until fusion begins. Energy generated by fusion provides thermal pressure to stop the collapse (“star”). If M < 0.08 MSun, degeneracy pressure stops gravitational con ...
... What prevents protostars from continually collapsing ever smaller? If M > 0.08 MSun, then gravitational contraction heats the core until fusion begins. Energy generated by fusion provides thermal pressure to stop the collapse (“star”). If M < 0.08 MSun, degeneracy pressure stops gravitational con ...
IAU-Perraut-2013 - Putting A Stars into Context
... (with contributions of Denis Mourard, Margarida Cunha, Nicolas Nardetto) ...
... (with contributions of Denis Mourard, Margarida Cunha, Nicolas Nardetto) ...
Lecture18
... Stars form in very large, cold interstellar clouds composed of molecular hydrogen and dust called, molecular clouds. These molecular clouds sit between the stars in the Galaxy. The are very cold (10 K) so we can only see them with infrared and radio telescopes ...
... Stars form in very large, cold interstellar clouds composed of molecular hydrogen and dust called, molecular clouds. These molecular clouds sit between the stars in the Galaxy. The are very cold (10 K) so we can only see them with infrared and radio telescopes ...
Testing
... A. They’re stuck to interstellar medium. B. Gravity of disk stars pulls them toward the disk. C. Halo stars knock them back into the disk. ...
... A. They’re stuck to interstellar medium. B. Gravity of disk stars pulls them toward the disk. C. Halo stars knock them back into the disk. ...
PPT presentation
... stars die very soon after reaching dlogM/dlogL = -1 observations of mass loss rates and/or location of the Mira variables tells you which stars are now dying. Mass loss rates are sensitive to a combination of R, L, and M such that low metallicity stars, smaller at a given L, M, reach higher L befo ...
... stars die very soon after reaching dlogM/dlogL = -1 observations of mass loss rates and/or location of the Mira variables tells you which stars are now dying. Mass loss rates are sensitive to a combination of R, L, and M such that low metallicity stars, smaller at a given L, M, reach higher L befo ...