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... in class) and the y axis is flux (don’t worry about those units!). Below each big plot is a zoomed-in view of the area of the spectrum around 6560 Ångstroms (i.e., 656 nm). Question 1 (1 point). Star #1 has a conspicuous Hα transition at 6563 Ångstroms. So, the zoomed-in view shows the Hα line for t ...
... in class) and the y axis is flux (don’t worry about those units!). Below each big plot is a zoomed-in view of the area of the spectrum around 6560 Ångstroms (i.e., 656 nm). Question 1 (1 point). Star #1 has a conspicuous Hα transition at 6563 Ångstroms. So, the zoomed-in view shows the Hα line for t ...
galctr
... --Same, but more extreme version of question for He I emission-line stars at 0.1 -0.5 pc from ctr. --Would need n > 1014 cm-3 at R=0.01 pc; n> 108 cm-3 at R=0.1 pc to form in situ given strong tidal gravity --> larger than any observed gas densities • Possible solutions include: Tidal heating of a ...
... --Same, but more extreme version of question for He I emission-line stars at 0.1 -0.5 pc from ctr. --Would need n > 1014 cm-3 at R=0.01 pc; n> 108 cm-3 at R=0.1 pc to form in situ given strong tidal gravity --> larger than any observed gas densities • Possible solutions include: Tidal heating of a ...
Part 1
... Below are two star photos taken six months apart and laid atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
... Below are two star photos taken six months apart and laid atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
بسم الله الرحمن الرحيم - Philadelphia University Jordan
... saw dark space. You might see that many stars look larger than others. You might see that some stars that look white are really red or blue. With bigger and bigger telescopes you can see more and more objects in the sky. And you can see those objects in more and more detail. But scientists believe t ...
... saw dark space. You might see that many stars look larger than others. You might see that some stars that look white are really red or blue. With bigger and bigger telescopes you can see more and more objects in the sky. And you can see those objects in more and more detail. But scientists believe t ...
Chapter 9 “The Family of Stars “
... spectroscopic: only by taking a spectrum can we see there are two stars. Astronomers wait to see how long it takes for spectral lines to return to their starting positions. - c. eclipsing: stars eclipse one another. Astronomers study the light curves from each star. ...
... spectroscopic: only by taking a spectrum can we see there are two stars. Astronomers wait to see how long it takes for spectral lines to return to their starting positions. - c. eclipsing: stars eclipse one another. Astronomers study the light curves from each star. ...
15.6 Planets Beyond the Solar System
... A substantial fraction of stars that have been measured have planets around them of the sort that can now be detected. They are mostly gas giants like Jupiter, but closer to star. Why didn’t our Jupiter migrate? Nearly all of these have been discovered using the radial velocity method. This method ( ...
... A substantial fraction of stars that have been measured have planets around them of the sort that can now be detected. They are mostly gas giants like Jupiter, but closer to star. Why didn’t our Jupiter migrate? Nearly all of these have been discovered using the radial velocity method. This method ( ...
Brock physics - Brock University
... (a) * electron degeneracy pressure. (b) neutron degeneracy pressure. (c) high pressure caused by the extremely high density and temperature of the core. (d) high pressure caused by intense gravity of the massive star. 33. Neutron stars have densities that are (a) about 10 times as dense as white dwa ...
... (a) * electron degeneracy pressure. (b) neutron degeneracy pressure. (c) high pressure caused by the extremely high density and temperature of the core. (d) high pressure caused by intense gravity of the massive star. 33. Neutron stars have densities that are (a) about 10 times as dense as white dwa ...
9 spectroscopic parallax
... We can measure apparent magnitude and spectral type. The main sequence lets us infer absolute magnitude from spectral type. Comparing apparent magnitude to absolute magnitude gives us distance. ...
... We can measure apparent magnitude and spectral type. The main sequence lets us infer absolute magnitude from spectral type. Comparing apparent magnitude to absolute magnitude gives us distance. ...
Stars: from Adolescence to Old Age
... terms of star lifetimes!) create conditions where the pressure and gravity are out of sync and the pulsations continue for a time • Larger, more luminous stars will pulsate with longer periods than the smaller, fainter stars – because gravity takes longer to pull the more extended outer layers of th ...
... terms of star lifetimes!) create conditions where the pressure and gravity are out of sync and the pulsations continue for a time • Larger, more luminous stars will pulsate with longer periods than the smaller, fainter stars – because gravity takes longer to pull the more extended outer layers of th ...
White Dwarfs and Neutron Stars
... • Neutron stars can form powerful jets of matter and energy • Previously only thought possible with black holes • Binary system with neutron star gaining matter from white dwarf companion’s atmosphere in an accretion disk • Neutron star is tiny compared to white dwarf but is very dense and about 14 ...
... • Neutron stars can form powerful jets of matter and energy • Previously only thought possible with black holes • Binary system with neutron star gaining matter from white dwarf companion’s atmosphere in an accretion disk • Neutron star is tiny compared to white dwarf but is very dense and about 14 ...
Lecture 22 - Seattle Central
... What are the main stages in a high mass star’s life? What happens in the core of a high mass star at the end of its life? Why does fusion stop at Iron in high mass stars? Where do elements heavier than Iron come from? What are the two possibilities when the electron degeneracy pressure in a high mas ...
... What are the main stages in a high mass star’s life? What happens in the core of a high mass star at the end of its life? Why does fusion stop at Iron in high mass stars? Where do elements heavier than Iron come from? What are the two possibilities when the electron degeneracy pressure in a high mas ...
answers2008_09_BC
... loses mass through stellar wind. Eventually all outer layers will be lost, forming a planetary nebula, and He fusion will stop; central carbon core will survive to radiate its stored heat as a white dwarf (bottom left of HRD) ...
... loses mass through stellar wind. Eventually all outer layers will be lost, forming a planetary nebula, and He fusion will stop; central carbon core will survive to radiate its stored heat as a white dwarf (bottom left of HRD) ...
Light-years
... Earth and sun b. The tilted orbit of the moon c. The moons period of revolution just equals its period of rotation d. Sunlight reflecting off Earth’s surface ...
... Earth and sun b. The tilted orbit of the moon c. The moons period of revolution just equals its period of rotation d. Sunlight reflecting off Earth’s surface ...
光學望遠鏡
... together or apart. The telescope lens is lined up on the pair and oriented using position wires that lie at right angles to the star separation. The movable wires are then adjusted to match the two star positions. The separation of the stars is then read off the instrument, and their true separation ...
... together or apart. The telescope lens is lined up on the pair and oriented using position wires that lie at right angles to the star separation. The movable wires are then adjusted to match the two star positions. The separation of the stars is then read off the instrument, and their true separation ...
Chapter 17 Measuring the Stars
... 17.5 The Hertzsprung-Russell Diagram Once many stars are plotted on an H-R diagram, a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence, as this is where most stars are. Also indicated is the white ...
... 17.5 The Hertzsprung-Russell Diagram Once many stars are plotted on an H-R diagram, a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence, as this is where most stars are. Also indicated is the white ...
Sample final exam
... 18. Two binary stars, each with a mass of 0.5 solar masses, orbit each other. Each has a semi-major axis of its orbit of 1.0 AU. What is the period (in years) of these stars? Essay section part one — Choose two of the following questions, and answer them in paragraph style or with drawings, as the ...
... 18. Two binary stars, each with a mass of 0.5 solar masses, orbit each other. Each has a semi-major axis of its orbit of 1.0 AU. What is the period (in years) of these stars? Essay section part one — Choose two of the following questions, and answer them in paragraph style or with drawings, as the ...
Part A
... • A star is a large ball of gas held together by gravity with a core so hot that nuclear fusion occurs. • Nuclear fusion occurs when the nuclei of several atoms combine into one larger ...
... • A star is a large ball of gas held together by gravity with a core so hot that nuclear fusion occurs. • Nuclear fusion occurs when the nuclei of several atoms combine into one larger ...
solutions
... pressure depends on the star’s surface gravity and therefore, roughly, on its size telling whether it is a giant, dwarf, or something in between. The size and surface brightness in turn yield the star’s luminosity (its total light output, or absolute magnitude) and often its evolutionary status (you ...
... pressure depends on the star’s surface gravity and therefore, roughly, on its size telling whether it is a giant, dwarf, or something in between. The size and surface brightness in turn yield the star’s luminosity (its total light output, or absolute magnitude) and often its evolutionary status (you ...