How Matter Emits Light: 2. Line Emission and
... does not have spectral line absorption does not have spectral line emission emits only x-rays emits only radio waves ...
... does not have spectral line absorption does not have spectral line emission emits only x-rays emits only radio waves ...
Teaching astrophysics in VCE Physics
... $ From these figures it was calculated that if the Sun was made of coal, it could burn for about 10,000 years - given a lot of oxygen! As life on the Earth seemed to be millions of years old this appeared to be a problem! $ Lord Kelvin and Hermann von Helmholtz suggested that the collapsing matter f ...
... $ From these figures it was calculated that if the Sun was made of coal, it could burn for about 10,000 years - given a lot of oxygen! As life on the Earth seemed to be millions of years old this appeared to be a problem! $ Lord Kelvin and Hermann von Helmholtz suggested that the collapsing matter f ...
Star formation and internal kinematics of irregular galaxies
... the relatively slow rotation of the Irregulars makes it difficult to generate strong densitywave shocks (Gallagher & Hunter 1984). Without this periodic stimulus acting upon upon clouds in their ISM (Elmegreen & Elmegreen 1983), other processes that trigger star ...
... the relatively slow rotation of the Irregulars makes it difficult to generate strong densitywave shocks (Gallagher & Hunter 1984). Without this periodic stimulus acting upon upon clouds in their ISM (Elmegreen & Elmegreen 1983), other processes that trigger star ...
Hertzsprung-Russell Diagram, Flux, Luminosity, Magnitude—10 Oct Outline •
... of classifying spectra. Hertzsprung‐Russell diagram ...
... of classifying spectra. Hertzsprung‐Russell diagram ...
MODELING PARALLAX
... The first method astronomers use to measure distances to stars is called parallax. Astronomers can measure parallax by measuring the position of a nearby star with respect to more distant stars behind it, then measuring that position again six months later when the Earth is on the opposite side of i ...
... The first method astronomers use to measure distances to stars is called parallax. Astronomers can measure parallax by measuring the position of a nearby star with respect to more distant stars behind it, then measuring that position again six months later when the Earth is on the opposite side of i ...
The Transfer Equation
... Teff = 4500 K. The two stars are of nearly equal V magnitude. What is the ratio of their fluxes at 2 microns? • In an eclipsing binary system, comprised of a B5V star at Teff = 16,000K and an F0III star at Teff = 7000K, the two stars are known to have nearly equal diameters. How deep will the primar ...
... Teff = 4500 K. The two stars are of nearly equal V magnitude. What is the ratio of their fluxes at 2 microns? • In an eclipsing binary system, comprised of a B5V star at Teff = 16,000K and an F0III star at Teff = 7000K, the two stars are known to have nearly equal diameters. How deep will the primar ...
mass loss of massive stars - of /proceedings
... Although short, the RSG phase strongly impacts on the neighbouring environment. In that phase, mass loss rates range from 10−7 to 10−4 M and the wind velocities are typically of 10 to 40 km s−1 . Hence, the wind density is about a thousand times larger than in the OB phase. Fig. 2 shows mass loss r ...
... Although short, the RSG phase strongly impacts on the neighbouring environment. In that phase, mass loss rates range from 10−7 to 10−4 M and the wind velocities are typically of 10 to 40 km s−1 . Hence, the wind density is about a thousand times larger than in the OB phase. Fig. 2 shows mass loss r ...
Dynamical Properties of Infrared Dark Clouds
... Infrared Dark Clouds (IRDCs) are a new class of interstellar clouds seen as dark extinction features against the bright Galactic background at mid-infrared (mid-IR) wavelengths. Studies thus far have shown these IRDCs to be dense (>105 cm-3), cold (<25 K), and to have very high column densities (>10 ...
... Infrared Dark Clouds (IRDCs) are a new class of interstellar clouds seen as dark extinction features against the bright Galactic background at mid-infrared (mid-IR) wavelengths. Studies thus far have shown these IRDCs to be dense (>105 cm-3), cold (<25 K), and to have very high column densities (>10 ...
The Milky Way
... that has been ionized by young, massive, hot stars. Their light is highly red-shifted because especially the star-forming regions are moving away from us at high speed. This is the red color of interstellar dust that is present in the molecular clouds out of which stars are formed. Star forming regi ...
... that has been ionized by young, massive, hot stars. Their light is highly red-shifted because especially the star-forming regions are moving away from us at high speed. This is the red color of interstellar dust that is present in the molecular clouds out of which stars are formed. Star forming regi ...
Europlanet 2007 Scientific Highlights (by Colin)
... – Fridlund (abstract 474) - summary of mission. So far, short sequence on one field (60 day). Many candidates. 1st papers due in 5-6 months. Mass function continues to small masses. – Barge et al. (316) - So far, 1 planet + 18 candidates. ...
... – Fridlund (abstract 474) - summary of mission. So far, short sequence on one field (60 day). Many candidates. 1st papers due in 5-6 months. Mass function continues to small masses. – Barge et al. (316) - So far, 1 planet + 18 candidates. ...
The Stars: Distance, Luminosity, Size
... What is the Hertzsprung-Russell Diagram? Why are most stars seen along the so-called main sequence? What makes more massive stars hotter and ...
... What is the Hertzsprung-Russell Diagram? Why are most stars seen along the so-called main sequence? What makes more massive stars hotter and ...
Star in a Box
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
Final Exam, Dec. 19, 2015 - Physics@Brock
... (b) some stars are circumpolar and some stars rise and set on the horizon. (c) all stars are circumpolar stars. 78. The celestial equator is (a) the projection of the Earth’s orbit on the celestial sphere. (b) the projection of the Earth’s equator on the celestial sphere. (c) the Sun’s apparent path ...
... (b) some stars are circumpolar and some stars rise and set on the horizon. (c) all stars are circumpolar stars. 78. The celestial equator is (a) the projection of the Earth’s orbit on the celestial sphere. (b) the projection of the Earth’s equator on the celestial sphere. (c) the Sun’s apparent path ...
Lecture Eleven (Powerpoint format)
... attempting at this very moment to measure the spacetime distortion produced by gravitational radiation. The strongest conceivable sources of gravitational radiation are coalescing binary black holes and neutron stars. Even with these incredibly intense and rare events, the expected signal is min ...
... attempting at this very moment to measure the spacetime distortion produced by gravitational radiation. The strongest conceivable sources of gravitational radiation are coalescing binary black holes and neutron stars. Even with these incredibly intense and rare events, the expected signal is min ...
Complex Processes in Simple Ices
... in our own solar system. Their evolution in the past set the stage for the chemistry we have today on this planet. Their evolution is right now setting the stage for the chemistry in extra-solar systems. Its investigation thus sets the stage for how life came in to being here and how likely it is to ...
... in our own solar system. Their evolution in the past set the stage for the chemistry we have today on this planet. Their evolution is right now setting the stage for the chemistry in extra-solar systems. Its investigation thus sets the stage for how life came in to being here and how likely it is to ...
Homologous Stellar Models and Polytropes Main Sequence Stars
... Figure 8.8. Occurrence of convective regions (gray shading) on the ZAMS in terms of fractional mass coordinate m/M as a function of stellar mass, for detailed stellar models with a composition X = 0.70, Z = 0.02. The solid (red) lines show the mass shells inside which 50% and 90% of the total lumino ...
... Figure 8.8. Occurrence of convective regions (gray shading) on the ZAMS in terms of fractional mass coordinate m/M as a function of stellar mass, for detailed stellar models with a composition X = 0.70, Z = 0.02. The solid (red) lines show the mass shells inside which 50% and 90% of the total lumino ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... our class will meet on Thursday, 9 October. (This makes up for one class day lost to Gustav last week.) • We will hold an additional makeup class on Saturday, 20 September! (This will account for the second class day lost to Gustav last week.) • Date of Exam #1 has been changed to Tuesday, 23 Septem ...
... our class will meet on Thursday, 9 October. (This makes up for one class day lost to Gustav last week.) • We will hold an additional makeup class on Saturday, 20 September! (This will account for the second class day lost to Gustav last week.) • Date of Exam #1 has been changed to Tuesday, 23 Septem ...
Why Aren`t All Galaxies Barred?
... have exactly circular orbits. If the orbit of a star is not perfectly circu lar, then it moves alternately inwards and outwards, whilst sometimes gaining on other nearby stars and at other times dropping behind. When all stars behave in this way, we say that there is some random motion (or velocity ...
... have exactly circular orbits. If the orbit of a star is not perfectly circu lar, then it moves alternately inwards and outwards, whilst sometimes gaining on other nearby stars and at other times dropping behind. When all stars behave in this way, we say that there is some random motion (or velocity ...
Lecture 10 Advanced Variable Star Stuff March 18 2003 8:00 PM
... A white dwarf is the remnant that is left after a star similar to our Sun dies. It blows off all of its outer layers and leaves behind a hot dense core. There is no more fuel for nuclear fusion (the elements left are mainly things like carbon and iron, not easy to fuse). If we add too much fuel, wha ...
... A white dwarf is the remnant that is left after a star similar to our Sun dies. It blows off all of its outer layers and leaves behind a hot dense core. There is no more fuel for nuclear fusion (the elements left are mainly things like carbon and iron, not easy to fuse). If we add too much fuel, wha ...
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.