WIRO: Spectral Analysis P1
... the core. So what we are able to “view” is absorption of photon energy, whereas in reality the energy was simply redirected. A lot of drops in a spectral graph means a lot of absorptions, and indicates the presence of a star versus a galaxy or quasar.. Absorption wavelength locations indicate elemen ...
... the core. So what we are able to “view” is absorption of photon energy, whereas in reality the energy was simply redirected. A lot of drops in a spectral graph means a lot of absorptions, and indicates the presence of a star versus a galaxy or quasar.. Absorption wavelength locations indicate elemen ...
gravitational collapse to black holes
... For general relativity, conformal maps are important since they leave the light-cone structure invariant - they therefore represent the overall causal structure of space-time while removing less important details ...
... For general relativity, conformal maps are important since they leave the light-cone structure invariant - they therefore represent the overall causal structure of space-time while removing less important details ...
Packet 3
... 7. Stars that are closer than 32.6 light-years away appear __________________________. Therefore those stars that are further than 32.6 light-years away appear ________________________. 8. How far away a star would be if it’s apparent magnitude and absolute magnitude were equal? _________ Match the ...
... 7. Stars that are closer than 32.6 light-years away appear __________________________. Therefore those stars that are further than 32.6 light-years away appear ________________________. 8. How far away a star would be if it’s apparent magnitude and absolute magnitude were equal? _________ Match the ...
Slides from Dr. Frank`s Lecture17
... 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becoming a red giant) Conclusion: Long period (wide) binaries may never become interacting while short period (close) binaries are ...
... 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becoming a red giant) Conclusion: Long period (wide) binaries may never become interacting while short period (close) binaries are ...
Modeling High-Mass X-ray Binary Formation in the Chandra Era Tim Linden
... Luminosity depends on: ...
... Luminosity depends on: ...
A Decade in the Life of the Massive Black-Hole Binary... Silas Laycock !
... • At each trial period we computed the mean count-rate in the phase range 0.4-0.6, which is mid-eclipse. • Chandra and XMM-Newton data were analyzed separately, yielding two sets of flux-minima, most of which are mutually exclusive. • The resulting best period, also found by the Lomb-Scargle peri ...
... • At each trial period we computed the mean count-rate in the phase range 0.4-0.6, which is mid-eclipse. • Chandra and XMM-Newton data were analyzed separately, yielding two sets of flux-minima, most of which are mutually exclusive. • The resulting best period, also found by the Lomb-Scargle peri ...
Measuring the Distances to the Stars: Parallax What sets the parallax limit?
... Hipparcos (1989-1993): 100-200 parsecs (1σ =1 milliarcsec = 1kpc) ...
... Hipparcos (1989-1993): 100-200 parsecs (1σ =1 milliarcsec = 1kpc) ...
Astrophysics notes
... Older cluster containing many more stars than open cluster and not containing massive O and B stars (too short lived). ...
... Older cluster containing many more stars than open cluster and not containing massive O and B stars (too short lived). ...
Lecture 10
... The dependence on M1/2 means that all these timescales are observationally feasible. However, lensing is a very rare event, all of the projects monitor millions of source stars to detect a handful of lensing events. ...
... The dependence on M1/2 means that all these timescales are observationally feasible. However, lensing is a very rare event, all of the projects monitor millions of source stars to detect a handful of lensing events. ...
Physics 1025: Lecture 17 Sun (cont.), Stellar Distances, Parallax
... the wavelength shift from the unshifted line λ. The star’s light will be blue-shifted if the star approaches earth. (Note in the case of an expanding nebula like the Crab Nebula, we assume it expands equally in all directions (i.e. spherically) and set VR= VT and can solve for the distance R to the ...
... the wavelength shift from the unshifted line λ. The star’s light will be blue-shifted if the star approaches earth. (Note in the case of an expanding nebula like the Crab Nebula, we assume it expands equally in all directions (i.e. spherically) and set VR= VT and can solve for the distance R to the ...
First Stars II
... density; cf. n~1022cm-3 for protostars) Overall evolution is similar to the 1D calculation. The collapse velocity is slower. (why? the effect of rotation, initial condition, turbulence) ...
... density; cf. n~1022cm-3 for protostars) Overall evolution is similar to the 1D calculation. The collapse velocity is slower. (why? the effect of rotation, initial condition, turbulence) ...
The Big Dipper Constellation
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
Winter Stargazing - Trimble County Schools
... • To find Auriga, first locate Orion. • Taurus is to the right (west) and just above these two, much higher in the sky, you will see Capella. • This star marks roughly the mid-point of the constellation, north to south. ...
... • To find Auriga, first locate Orion. • Taurus is to the right (west) and just above these two, much higher in the sky, you will see Capella. • This star marks roughly the mid-point of the constellation, north to south. ...
the star
... Proxima Centauri is a faint red star that orbits Alpha-Centauri A and B with a period of about one million years. Proxima Centauri is 4.22 light years from the Earth (now) and about 0.24 light years from Alpha-Centauri A and B. • Alpha-Centauri A and B – a double star system with a period of about ...
... Proxima Centauri is a faint red star that orbits Alpha-Centauri A and B with a period of about one million years. Proxima Centauri is 4.22 light years from the Earth (now) and about 0.24 light years from Alpha-Centauri A and B. • Alpha-Centauri A and B – a double star system with a period of about ...
Stars and Constellations
... For the people in the Native American southwest, the sky is not something remote from Earth. Rather, it is a unifying whole, both a window into the universe and an instrument for understanding and measuring its rhythms. Indian people have been watching the sky for many generations and applying its s ...
... For the people in the Native American southwest, the sky is not something remote from Earth. Rather, it is a unifying whole, both a window into the universe and an instrument for understanding and measuring its rhythms. Indian people have been watching the sky for many generations and applying its s ...
Stars
... III. Life cycle of Sun C. Becoming a Red Giant 1. After about 10 billion years, hydrogen is used up 2. Core of star is made of He 3. Layer of gas surrounding core does fusion, causing gases to expand and ...
... III. Life cycle of Sun C. Becoming a Red Giant 1. After about 10 billion years, hydrogen is used up 2. Core of star is made of He 3. Layer of gas surrounding core does fusion, causing gases to expand and ...
V - ESO
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
Here
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.