12.1 Introduction
... The evolution of more massive stars on the main sequence differs from that of solar mass stars in one important aspect: stars more massive than the Sun have convective cores, as we saw in Lecture 8.3.1. The timescale for convection, defined as the time it takes for a convective element to travel one ...
... The evolution of more massive stars on the main sequence differs from that of solar mass stars in one important aspect: stars more massive than the Sun have convective cores, as we saw in Lecture 8.3.1. The timescale for convection, defined as the time it takes for a convective element to travel one ...
Chapter 16
... 1. The density wave theory was first proposed by Lindblad in 1960. It is a model for spiral galaxies that proposes that the arms are the result of density waves sweeping around the galaxy. 2. A density wave is a wave in which areas of high and low pressure move through the medium. 3. The density wav ...
... 1. The density wave theory was first proposed by Lindblad in 1960. It is a model for spiral galaxies that proposes that the arms are the result of density waves sweeping around the galaxy. 2. A density wave is a wave in which areas of high and low pressure move through the medium. 3. The density wav ...
Stellar Evolution 1
... Life tracks for protostars Star birth similar for all stars, but massive stars pass through the stages faster ...
... Life tracks for protostars Star birth similar for all stars, but massive stars pass through the stages faster ...
Astronomy 730 / Galaxies
... zb. At t = t0 the boundary conditions are that σz(R, t0) = σz(0, t0) exp(−R/2hR) and hz(R, t0) = constant. If we take σz(R0,t0) = 20 km/s, we know that hz(R, t0) = 350 pc, again based on the old stars in the thin disk in the solar neighborhood. (c) Equate σz(R, t0) = σz(0, t0) exp(-R/2hR) with σz(R, ...
... zb. At t = t0 the boundary conditions are that σz(R, t0) = σz(0, t0) exp(−R/2hR) and hz(R, t0) = constant. If we take σz(R0,t0) = 20 km/s, we know that hz(R, t0) = 350 pc, again based on the old stars in the thin disk in the solar neighborhood. (c) Equate σz(R, t0) = σz(0, t0) exp(-R/2hR) with σz(R, ...
script (powerpoint)
... If there is no bright (mag ~ 14-15) nearby star then you must use an artificial star or „laser guide star“. All laser guide AO systems use a sodium laser tuned to Na 5890 Å pointed to the 11.5 km thick layer of enhanced sodium at an altitude of ...
... If there is no bright (mag ~ 14-15) nearby star then you must use an artificial star or „laser guide star“. All laser guide AO systems use a sodium laser tuned to Na 5890 Å pointed to the 11.5 km thick layer of enhanced sodium at an altitude of ...
Molecular Cloud www.AssignmentPoint.com A molecular cloud
... of the volume of the interstellar medium (ISM), yet it is also the densest part of the medium, comprising roughly half of the total gas mass interior to the Sun's galactic orbit. The bulk of the molecular gas is contained in a ring between 3.5 and 7.5 kiloparsecs (11,000 and 24,000 light-years) from ...
... of the volume of the interstellar medium (ISM), yet it is also the densest part of the medium, comprising roughly half of the total gas mass interior to the Sun's galactic orbit. The bulk of the molecular gas is contained in a ring between 3.5 and 7.5 kiloparsecs (11,000 and 24,000 light-years) from ...
Slides from the talk
... The galaxy cluster 1E 0657-56, known as the "bullet cluster“. A mere 3.4 billion light-years away, the bullet cluster's individual galaxies are seen in the optical image data, but their total mass adds up to far less than the mass of the cluster's two clouds of hot x-ray emitting gas shown in red. R ...
... The galaxy cluster 1E 0657-56, known as the "bullet cluster“. A mere 3.4 billion light-years away, the bullet cluster's individual galaxies are seen in the optical image data, but their total mass adds up to far less than the mass of the cluster's two clouds of hot x-ray emitting gas shown in red. R ...
The ages of pre-main-sequence stars
... the hydrostatic inner regions using the methods normally employed in stellar evolution and so, with appropriate boundary conditions, approximate a forming star. Indeed, this kind of premain-sequence theory can be said to have begun alongside stellar evolution itself with the work of Henyey, Lelevier ...
... the hydrostatic inner regions using the methods normally employed in stellar evolution and so, with appropriate boundary conditions, approximate a forming star. Indeed, this kind of premain-sequence theory can be said to have begun alongside stellar evolution itself with the work of Henyey, Lelevier ...
Exploring Solar Systems Across the Universe
... small grains of dust within the disk collided, stuck ...
... small grains of dust within the disk collided, stuck ...
Page 25 - Types of Galaxies
... • They tend to be smaller objects that are without definite shape and tend to have very hot newer stars mixed in with lots of gas and dust. • These galaxies often have active regions of star formation. Sometimes the irregular shape of these galaxies results from interactions or collisions between ga ...
... • They tend to be smaller objects that are without definite shape and tend to have very hot newer stars mixed in with lots of gas and dust. • These galaxies often have active regions of star formation. Sometimes the irregular shape of these galaxies results from interactions or collisions between ga ...
Stars: Their Life and Afterlife
... they continue to shrink and glow faintly via KH contraction for many years. The Sun began its main-sequence life with a composition of • 74% hydrogen • 25% helium • ~1% heavier elements, or “metals” After ~4.6 billion years of burning hydrogen in its core, the Sun’s core is now ~65% helium, but enou ...
... they continue to shrink and glow faintly via KH contraction for many years. The Sun began its main-sequence life with a composition of • 74% hydrogen • 25% helium • ~1% heavier elements, or “metals” After ~4.6 billion years of burning hydrogen in its core, the Sun’s core is now ~65% helium, but enou ...
Fate of Stars
... Stars with larger sizes are brighter then a smaller star with the same surface temperature ...
... Stars with larger sizes are brighter then a smaller star with the same surface temperature ...
W. M. White Geochemistry Chapter 10: Cosmochemistry
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
Galactic planetary science
... Water vapour appears to be ubiquitous in the atmospheres of transiting hotJupiters with temperatures between 800 and 2200 K observed to date (Barman, 2007; Tinetti et al., 2007b; Grillmair et al., 2008; Beaulieu et al., 2010; Swain et al., 2008; Crouzet et al., 2012; Deming et al., 2013; Birkby et a ...
... Water vapour appears to be ubiquitous in the atmospheres of transiting hotJupiters with temperatures between 800 and 2200 K observed to date (Barman, 2007; Tinetti et al., 2007b; Grillmair et al., 2008; Beaulieu et al., 2010; Swain et al., 2008; Crouzet et al., 2012; Deming et al., 2013; Birkby et a ...
Galaxy Structure
... Dame et al (1987, 1999) have combined large-scale surveys of the 12CO(1–0) integrated line intensity of the entire Galactic plane and specific nearby clouds to produce a panorama of the entire Milky Way in molecular gas at an angular resolution of Jº. Their compilation exhibits a sky coverage and re ...
... Dame et al (1987, 1999) have combined large-scale surveys of the 12CO(1–0) integrated line intensity of the entire Galactic plane and specific nearby clouds to produce a panorama of the entire Milky Way in molecular gas at an angular resolution of Jº. Their compilation exhibits a sky coverage and re ...
Inquiry Activity - Ball State University
... The astronomers of old did not realize that it only appears as though everything rotates around the earth. What they did not consider was whether the Earth itself was rotating about its own axis. This was not obvious to them, and it is not obvious to us because it does not feel like the Earth is sp ...
... The astronomers of old did not realize that it only appears as though everything rotates around the earth. What they did not consider was whether the Earth itself was rotating about its own axis. This was not obvious to them, and it is not obvious to us because it does not feel like the Earth is sp ...
EASTERN ARIZONA COLLEGE Lab - Introduction to Astronomy
... learner can identify the motion of planets along the ecliptic ...
... learner can identify the motion of planets along the ecliptic ...
File
... The star is new and it doesn't understand it's solar system. What should they do? How can they solve their problem? They shouldn't be worried, it is all normal. Why should they do that? What facts can we give to them to reinforce our answer? The objects revolving around the star are probably planets ...
... The star is new and it doesn't understand it's solar system. What should they do? How can they solve their problem? They shouldn't be worried, it is all normal. Why should they do that? What facts can we give to them to reinforce our answer? The objects revolving around the star are probably planets ...
SECTION28.1 Formation of the Solar System
... a. the nightly motion of the stars b. the rising and setting of the Sun c. the retrograde motion of planets d. the occurrence of meteor showers ...
... a. the nightly motion of the stars b. the rising and setting of the Sun c. the retrograde motion of planets d. the occurrence of meteor showers ...
Astronomy in 1936 The History of the Universe
... • Molecular clouds form on inner edges of spiral arms. • HI gas flow shows discontinuity due to shocks at inner edges of spiral arms. • Bright young stars also in narrow arms. • Observed width ∆θ ~ t*(Ω - Ωp) , as predicted. ...
... • Molecular clouds form on inner edges of spiral arms. • HI gas flow shows discontinuity due to shocks at inner edges of spiral arms. • Bright young stars also in narrow arms. • Observed width ∆θ ~ t*(Ω - Ωp) , as predicted. ...
EXPLORATION OF THE KUIPER BELT BY HIGH
... KBOs down to objects of 1 km radius leads to 1011 KBOs with a total mass of only 0.1 Mo (Gladman et al. 2001). In contrast, a simple extrapolation of the surface mass density of the solar system outside 35 AU yields several Earth masses. Moreover, KBO accretion models require an initial Kuiper Belt ...
... KBOs down to objects of 1 km radius leads to 1011 KBOs with a total mass of only 0.1 Mo (Gladman et al. 2001). In contrast, a simple extrapolation of the surface mass density of the solar system outside 35 AU yields several Earth masses. Moreover, KBO accretion models require an initial Kuiper Belt ...