ASTR 553/554 (1) : Questions
... b. What's the surface brightness, I(0), at the center of the Milky Way disk, and what's the disk's total luminosity in LV, . c. Using MV, = 4.82, calculate the Milky Way's absolute magnitude, MV. If viewed from Virgo (distance 15 Mpc) what would its apparent magnitude, mV be? Would an Alien equivale ...
... b. What's the surface brightness, I(0), at the center of the Milky Way disk, and what's the disk's total luminosity in LV, . c. Using MV, = 4.82, calculate the Milky Way's absolute magnitude, MV. If viewed from Virgo (distance 15 Mpc) what would its apparent magnitude, mV be? Would an Alien equivale ...
Instruments and Science Programs - California State University
... companion star, if one is present. Last fall, Fresno State grad student Scott Endler discovered that PB 7032 is variable: one night it was clearly two magnitudes fainter than on the other four nights Scott observed it. We plan detailed observations this summer, when PB 7032 emerges from behind the S ...
... companion star, if one is present. Last fall, Fresno State grad student Scott Endler discovered that PB 7032 is variable: one night it was clearly two magnitudes fainter than on the other four nights Scott observed it. We plan detailed observations this summer, when PB 7032 emerges from behind the S ...
Properties of stars
... How bright a star appears depends on both how much light it releases (its actual brightness or luminosity) and how far away it is (distance) according to the inverse square law ...
... How bright a star appears depends on both how much light it releases (its actual brightness or luminosity) and how far away it is (distance) according to the inverse square law ...
LAB #6 - GEOCITIES.ws
... PRE-LAB WARMUP QUESTION: A star gives out more blue light than yellow. Thus its B-V is (positive, negative, zero). The most likely spectral type for this star is (B, K, M). When one constructs an HR Diagram from the apparent V magnitude versus the B-V color index of a cluster of stars, one finds tha ...
... PRE-LAB WARMUP QUESTION: A star gives out more blue light than yellow. Thus its B-V is (positive, negative, zero). The most likely spectral type for this star is (B, K, M). When one constructs an HR Diagram from the apparent V magnitude versus the B-V color index of a cluster of stars, one finds tha ...
Rogava_Course_-_First_lecture
... event seen around 1843. In a few years, it produced almost as much visible light as a supernova explosion, but it survived. ...
... event seen around 1843. In a few years, it produced almost as much visible light as a supernova explosion, but it survived. ...
What are the Spectral Lines? - University of Texas Astronomy Home
... - real knowledge only due to hard facts, e.g., laboratory science, measurements • claimed ...
... - real knowledge only due to hard facts, e.g., laboratory science, measurements • claimed ...
Friday, April 25 - Otterbein University
... • “yard-sticks” for distance measurement • Cepheids in Andromeda Galaxies established the “extragalacticity” of this “nebula” ...
... • “yard-sticks” for distance measurement • Cepheids in Andromeda Galaxies established the “extragalacticity” of this “nebula” ...
20040907103511001-148699
... Differential-rotation decay Rotation of solar core is slow and uniform Rotation period has increased by factor of 10 during life Viscosity too small to reduce rotation homogeneously throughout the Sun Magnetic Ap stars rotate much slower than „normal“ A stars Did MRI reduce the internal rot ...
... Differential-rotation decay Rotation of solar core is slow and uniform Rotation period has increased by factor of 10 during life Viscosity too small to reduce rotation homogeneously throughout the Sun Magnetic Ap stars rotate much slower than „normal“ A stars Did MRI reduce the internal rot ...
Notes 4, p. 1-3
... ⊲ In a non-equilibrium state, there is not enough outward force to oppose the gravitational collapse so the star begins to contract ⊲ For the star to contract, gravitational potential energy must be lost; in this case it goes into heating the star at a smaller radius (keeping the star shining) ⊲ The ...
... ⊲ In a non-equilibrium state, there is not enough outward force to oppose the gravitational collapse so the star begins to contract ⊲ For the star to contract, gravitational potential energy must be lost; in this case it goes into heating the star at a smaller radius (keeping the star shining) ⊲ The ...
Teaching astrophysics in VCE Physics
... that all stars begin their lives on the main sequence. New clusters have more relatively large stars but older ones have relatively few - they have burnt out. $ So we deduce that large stars die young, becoming giants or supergiants for a relatively short time, and then moving downward to become dwa ...
... that all stars begin their lives on the main sequence. New clusters have more relatively large stars but older ones have relatively few - they have burnt out. $ So we deduce that large stars die young, becoming giants or supergiants for a relatively short time, and then moving downward to become dwa ...
RIPL Radio Interferometric Planet Search
... Sensitivity is limited by the short lever arm of VLBA observations: ~10 days RIPL will extend this lever arm by factor of 100 ...
... Sensitivity is limited by the short lever arm of VLBA observations: ~10 days RIPL will extend this lever arm by factor of 100 ...
Name: Period: ______ Date: Fission and Fusion Simulations Fission
... Fusion Go back to this page and watch the video about fusion http://www.atomicarchive.com/Movies/ 20. What particles and how many of each does the reaction start with? ...
... Fusion Go back to this page and watch the video about fusion http://www.atomicarchive.com/Movies/ 20. What particles and how many of each does the reaction start with? ...
YSO/PMS disk types, time-scales and evolution from 1
... timescales preferential for large ‘Jupiter’ planets that RESULT! ...
... timescales preferential for large ‘Jupiter’ planets that RESULT! ...
File - Adriana Romo
... Scientist: White dwarfs are about the size of earth or 10,000 km. In diameter, very hot and very dim. Interviewer: What is the surface temperature of a white dwarf? Scientist: Its about 20,000 degrees Celsius. Interviewer: What would happen to the white dwarf’s core? Scientist: The core will have no ...
... Scientist: White dwarfs are about the size of earth or 10,000 km. In diameter, very hot and very dim. Interviewer: What is the surface temperature of a white dwarf? Scientist: Its about 20,000 degrees Celsius. Interviewer: What would happen to the white dwarf’s core? Scientist: The core will have no ...
The Galaxy Presentation 2011
... - The motions of gas and stars in SgrA indicate that it contains a few million solar masses in a region no bigger than 3 lightyears. - Astronomers suspect SgrA is a black hole weighing 2.5 million solar masses; this is like no other observed black hole. - Other black hole candidates like Cygnus X-1 ...
... - The motions of gas and stars in SgrA indicate that it contains a few million solar masses in a region no bigger than 3 lightyears. - Astronomers suspect SgrA is a black hole weighing 2.5 million solar masses; this is like no other observed black hole. - Other black hole candidates like Cygnus X-1 ...
Stellar Structure - Astronomy Centre
... • But actually a plasma – highly ionised gas, so that particle size ~ nuclear radius << typical separation (~ atomic radius). • Hence stellar material behaves like an ideal gas (plus radiation pressure) – see blackboard ...
... • But actually a plasma – highly ionised gas, so that particle size ~ nuclear radius << typical separation (~ atomic radius). • Hence stellar material behaves like an ideal gas (plus radiation pressure) – see blackboard ...
Lecture Eight (Powerpoint format) - Flash
... parent gas cloud (sometimes called a “molecular cloud core”) without turbulence or magnetic fields. Initially, before the star has formed, the parent gas cloud is a state of hydrostatic balance. ...
... parent gas cloud (sometimes called a “molecular cloud core”) without turbulence or magnetic fields. Initially, before the star has formed, the parent gas cloud is a state of hydrostatic balance. ...
The Sun (power point) by Ms. Kimball the_sun_pp
... • Although the nuclear output of the sun is not entirely consistent, each second the Sun converts about 600,000,000 tons of hydrogen nuclei into helium nuclei. • These fusion reactions convert part of these atoms' mass (roughly 4 million tons) into energy, and release an enormous amount of this hea ...
... • Although the nuclear output of the sun is not entirely consistent, each second the Sun converts about 600,000,000 tons of hydrogen nuclei into helium nuclei. • These fusion reactions convert part of these atoms' mass (roughly 4 million tons) into energy, and release an enormous amount of this hea ...
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.