FP11: DRAKE et al. - Astronomical Institute WWW Homepage
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
Jeans Length
... Lecture 6: Jeans mass & length Anisotropies in the CMB temperature density ripples ...
... Lecture 6: Jeans mass & length Anisotropies in the CMB temperature density ripples ...
Maximum Mass Limit of Stars on the Main Sequence
... of these objects. Essentially, there are no conclusive observations that indicate whether a slow or a fast method applies to this type of stellar formation. Regardless of the approach, some of the gas in these filaments can become gravitationally bound and begin the collapse necessary to begin the ...
... of these objects. Essentially, there are no conclusive observations that indicate whether a slow or a fast method applies to this type of stellar formation. Regardless of the approach, some of the gas in these filaments can become gravitationally bound and begin the collapse necessary to begin the ...
Re-distribution of the planetary material between the Sun and giant
... is believed that it represents the zone of gravitation equilibrium between the Sun and the Jupiter took place at time of their concurrent growth. The position of this zone was not constant. The Sun gravitation attraction grew more quickly, than the Jupiter one. Because of that the equilibrium zone m ...
... is believed that it represents the zone of gravitation equilibrium between the Sun and the Jupiter took place at time of their concurrent growth. The position of this zone was not constant. The Sun gravitation attraction grew more quickly, than the Jupiter one. Because of that the equilibrium zone m ...
Parent stars of extrasolar planets III: ρ1 Cancri Revisited
... the universe! An accurate age estimate will allow us to compare ρ1 Cnc’s metallicity to Galactic chemical evolution predictions, so that we can determine if it really is anomalous. Such comparisons will also help to decide between the two main hypotheses proposed in Papers I & II to account for the ...
... the universe! An accurate age estimate will allow us to compare ρ1 Cnc’s metallicity to Galactic chemical evolution predictions, so that we can determine if it really is anomalous. Such comparisons will also help to decide between the two main hypotheses proposed in Papers I & II to account for the ...
Chapter 10 Late evolution of low- and intermediate
... radial pulsations, they are known as Mira variables (see Fig. 9.10). An observational correlation exists between the pulsation period and the mass-loss rate. As a star evolves towards larger radii along the AGB, the pulsation period increases (why?) and so does the mass-loss rate, from ∼ 10−7 M⊙ /yr ...
... radial pulsations, they are known as Mira variables (see Fig. 9.10). An observational correlation exists between the pulsation period and the mass-loss rate. As a star evolves towards larger radii along the AGB, the pulsation period increases (why?) and so does the mass-loss rate, from ∼ 10−7 M⊙ /yr ...
MACHOs
... o divide luminosity of galaxy/luminosity of star to find number of stars x mass of average star = mass of galaxy o FOUND DARK MATTER – because dark matter doesn’t emit light, it doesn’t give luminosity, so the difference in the two values is due to dark matter 99% of matter in the galaxy is dark ...
... o divide luminosity of galaxy/luminosity of star to find number of stars x mass of average star = mass of galaxy o FOUND DARK MATTER – because dark matter doesn’t emit light, it doesn’t give luminosity, so the difference in the two values is due to dark matter 99% of matter in the galaxy is dark ...
Variability of solar/stellar activity and magnetic field and its influence... planetary atmosphere evolution
... • Young stars rotate more rapidly and have an internal magnetic dynamo that is more efficient than that of the present-day Sun. This results in stronger surface magnetic fields and/or higher surface magnetic filling factors which induce enhanced “activity” in all its variations, from larger surface ...
... • Young stars rotate more rapidly and have an internal magnetic dynamo that is more efficient than that of the present-day Sun. This results in stronger surface magnetic fields and/or higher surface magnetic filling factors which induce enhanced “activity” in all its variations, from larger surface ...
Unit 8 Chapter 30 Stars, Galaxies and the Universe
... These ripples are irregularities in the cosmic background radiation, which were caused by small fluctuations in the distribution of matter in the early universe. The ripples are thought to indicate the first stages in the formation of the universe's first galaxies. ...
... These ripples are irregularities in the cosmic background radiation, which were caused by small fluctuations in the distribution of matter in the early universe. The ripples are thought to indicate the first stages in the formation of the universe's first galaxies. ...
Astrophysics
... includes observations with space-based observatories, analytical and numerical modeling, and large-scale numerical simulations. In addition to work described below, topics include Big Bang nucleosynthesis, galactic chemical evolution, stellar winds, interacting binary stars, accretion disks, and pul ...
... includes observations with space-based observatories, analytical and numerical modeling, and large-scale numerical simulations. In addition to work described below, topics include Big Bang nucleosynthesis, galactic chemical evolution, stellar winds, interacting binary stars, accretion disks, and pul ...
Head-On Collision of Neutron Stars As A Thought Experiment
... energy. The configuration is not in equilibrium following the passage of the initial recoil shocks, but undergoes oscillations, damped by acoustic (viscous) dissipation and gravitational radiation reaction forces. Only a small fraction of the total rest mass escapes from the system and an even small ...
... energy. The configuration is not in equilibrium following the passage of the initial recoil shocks, but undergoes oscillations, damped by acoustic (viscous) dissipation and gravitational radiation reaction forces. Only a small fraction of the total rest mass escapes from the system and an even small ...
Hubble Does Double-Duty Science: Finding Planets and
... approximate location of a solar-like star ...
... approximate location of a solar-like star ...
ESO telescopes
... temperatures between 2,000 and 1,500 K. Therefore, IRAS 13481-6124 is following the size-luminosity relation22, which is well established for low- to intermediate mass ...
... temperatures between 2,000 and 1,500 K. Therefore, IRAS 13481-6124 is following the size-luminosity relation22, which is well established for low- to intermediate mass ...
Lesson 1-0 Slides The Cosmic Landscape
... How can we measure huge distances? A clue—the common flashlight Speed of light—a way to measure distances in space ...
... How can we measure huge distances? A clue—the common flashlight Speed of light—a way to measure distances in space ...
A Note on the Mixing Length Theory and Massive Star Evolution
... Figure 1 displays (in dotted lines) 3 envelope models of a 20 M with effective temperatures: 3600 K (top panels), 3900 K (middle panels) and 4200 K (lower panels). The dotted lines represent the results obtained with the convective envelope for late type supergiants following the original MLT (Vite ...
... Figure 1 displays (in dotted lines) 3 envelope models of a 20 M with effective temperatures: 3600 K (top panels), 3900 K (middle panels) and 4200 K (lower panels). The dotted lines represent the results obtained with the convective envelope for late type supergiants following the original MLT (Vite ...
Great Migrations & other natural history tales
... Planetary rings are also accretion disks, sort of. They are special: their thickness is extremely small: z/r = 10 m/ 66000 km ~ 1e-6, which makes them rather slowly accreting disks. ...
... Planetary rings are also accretion disks, sort of. They are special: their thickness is extremely small: z/r = 10 m/ 66000 km ~ 1e-6, which makes them rather slowly accreting disks. ...
... their very nature and rarity stir the imagination of all. Nobody can remain unaffected by a total solar eclipse, which is a life time experience or a Transit of Venus which come in pair after a span of over hundred years. Such events raise many questions in the minds of those who are not familiar wi ...
HEPAP Subpanel
... The development of this underground facility and its associated surface facilities is funded by ~$50M from various resources in Canada and in the Province of Ontario. SNOLAB will be developed near the existing SNO experiment with a joint clean area encompassing the full facility. The establishment o ...
... The development of this underground facility and its associated surface facilities is funded by ~$50M from various resources in Canada and in the Province of Ontario. SNOLAB will be developed near the existing SNO experiment with a joint clean area encompassing the full facility. The establishment o ...
1Lec_1 - The University of Texas at Dallas
... Fear Not: The detailed information that follows in slides #14 - #26 will “not be on the test.” We are going to go through it because I believe that a Biology major should have been at least briefly exposed to this basic information!) J G Burr, 08/23/15 ...
... Fear Not: The detailed information that follows in slides #14 - #26 will “not be on the test.” We are going to go through it because I believe that a Biology major should have been at least briefly exposed to this basic information!) J G Burr, 08/23/15 ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... – After core no longer contains helium, star may enter “asymptotic giant branch (AGB)” phase; helium continues to burn in a shell that surrounds an inert C & O core – As AGB star, star’s radius is 1 AU or larger! – Outer envelope ejected (nonviolently) to reveal the hot, inner core planetary nebul ...
... – After core no longer contains helium, star may enter “asymptotic giant branch (AGB)” phase; helium continues to burn in a shell that surrounds an inert C & O core – As AGB star, star’s radius is 1 AU or larger! – Outer envelope ejected (nonviolently) to reveal the hot, inner core planetary nebul ...
Practical Class - Physics and Astronomy
... Release of Cloudy Ferland 2003, ARA&A, 41, 517, Quantitative Spectroscopy of Photoionized Clouds ...
... Release of Cloudy Ferland 2003, ARA&A, 41, 517, Quantitative Spectroscopy of Photoionized Clouds ...