Astronomy Assignment #1
... Review Questions from the first half of Chapter 13: Lives and Deaths of Stars 1. What fundamental property of stars determines their evolution? Mass is the fundamental property that determines the evolution of stars. The mass of a star determines the central pressure of the star which in turn is the ...
... Review Questions from the first half of Chapter 13: Lives and Deaths of Stars 1. What fundamental property of stars determines their evolution? Mass is the fundamental property that determines the evolution of stars. The mass of a star determines the central pressure of the star which in turn is the ...
Phys 100 – Astronomy (Dr. Ilias Fernini) Review Questions for
... e. smaller than expected because the magnetic field is so strong. 54. A neutron star is expected to spin rapidly because * a. they conserved angular momentum when they collapsed. b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the ...
... e. smaller than expected because the magnetic field is so strong. 54. A neutron star is expected to spin rapidly because * a. they conserved angular momentum when they collapsed. b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the ...
Lecture 10 - University of Minnesota
... shows how the minimum mass of a star forming cloud varies with density. Following these examples (especially the ones on page 533), figure out how dense the could would have to be to form a single, 1 solar mass star. What does this say about why stars usually form in clusters? ...
... shows how the minimum mass of a star forming cloud varies with density. Following these examples (especially the ones on page 533), figure out how dense the could would have to be to form a single, 1 solar mass star. What does this say about why stars usually form in clusters? ...
Document
... Alnilam: "Epsilon Orionis," is a blue supergiant, despite being nearly twice as far from the Sun as Mintake and Alnitak, the other two belt stars. ...
... Alnilam: "Epsilon Orionis," is a blue supergiant, despite being nearly twice as far from the Sun as Mintake and Alnitak, the other two belt stars. ...
Westerlund 1 : A Super-Star Cluster within the Milky Way
... identified in the Milky Way. Wd1 hosts a rich population of OB supergiants, Wolf-Rayet stars, Luminous Blue Variables, Yellow Hypergiants and Red Supergiants, from which we infer an age of 3-5Myr. For an adopted Kroupa IMF we derive a mass of 105 M and radius of 0.3pc for an estimated distance of 2 ...
... identified in the Milky Way. Wd1 hosts a rich population of OB supergiants, Wolf-Rayet stars, Luminous Blue Variables, Yellow Hypergiants and Red Supergiants, from which we infer an age of 3-5Myr. For an adopted Kroupa IMF we derive a mass of 105 M and radius of 0.3pc for an estimated distance of 2 ...
The Main Features of the X
... The Main Features Supernovae (SNe), Supernova Remnants (SNRs), and Superbubbles ...
... The Main Features Supernovae (SNe), Supernova Remnants (SNRs), and Superbubbles ...
HW7-3
... (261) P 1: In the Figure 12-2, how much of the sun’s mass is hotter than 13,000,000 K? About 7.3%. Probably a bit more. L2L 1: In the photograph of the Pleiades on page 255, there are no bright red stars. Use the H-R diagram to explain why the brightest stars are blue. Have there ever been bright re ...
... (261) P 1: In the Figure 12-2, how much of the sun’s mass is hotter than 13,000,000 K? About 7.3%. Probably a bit more. L2L 1: In the photograph of the Pleiades on page 255, there are no bright red stars. Use the H-R diagram to explain why the brightest stars are blue. Have there ever been bright re ...
THE SPECTRA OF FIVE IRREGULAR VARIABLE STARS George H
... combination spectra, such as AX Persei, CI Cygni, and Ζ Andromedae. S. FN Sagittarii.—This star has been classified as "novalike'' on the strength of a flare-up to magnitude 9 that was observed in 1925.8 When the Lick spectrograms (listed in Table IV) ...
... combination spectra, such as AX Persei, CI Cygni, and Ζ Andromedae. S. FN Sagittarii.—This star has been classified as "novalike'' on the strength of a flare-up to magnitude 9 that was observed in 1925.8 When the Lick spectrograms (listed in Table IV) ...
Student Exploration Sheet: Growing Plants
... An absorption spectrum is created when light from a star passes through cooler gases surrounding the star. The dark lines correspond to colors of light that are absorbed by the atoms in these gases. Blueshift – the phenomenon in which light from a source that is moving toward an observer is shifted ...
... An absorption spectrum is created when light from a star passes through cooler gases surrounding the star. The dark lines correspond to colors of light that are absorbed by the atoms in these gases. Blueshift – the phenomenon in which light from a source that is moving toward an observer is shifted ...
Indoor lab #1: The Hertzsprung-Russel Diagram and Selection Effects
... a) the average distance of all the stars in your table: b) the number of and average distance of the red giant stars (stars of type 1) c) the number of and average distance of the bluer main sequence stars (stars of type 2) d) the number of and average distance of the redder main sequence stars (sta ...
... a) the average distance of all the stars in your table: b) the number of and average distance of the red giant stars (stars of type 1) c) the number of and average distance of the bluer main sequence stars (stars of type 2) d) the number of and average distance of the redder main sequence stars (sta ...
Exam #2 Solutions
... The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to the Sun. The main sequence stars will have lifetimes less than 1 billion years and the giants are at the end of their lives with perhaps as little as10 ...
... The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to the Sun. The main sequence stars will have lifetimes less than 1 billion years and the giants are at the end of their lives with perhaps as little as10 ...
Document
... in SNRs, GMCs, Galactic Plane/Bulge, Nearby galaxies, Nearby Clusters Separation of electron contribution (brems. and IC) and proton contribution (pi-0) is important. Association of SNRs, history of the galaxy or the cluster Even in galactic level, the total energy of cosmic-ray is non-negligibl ...
... in SNRs, GMCs, Galactic Plane/Bulge, Nearby galaxies, Nearby Clusters Separation of electron contribution (brems. and IC) and proton contribution (pi-0) is important. Association of SNRs, history of the galaxy or the cluster Even in galactic level, the total energy of cosmic-ray is non-negligibl ...
DTU_9e_ch13
... A pulsar is a rapidly rotating neutron star with a powerful magnetic field that makes it a source of periodic radio and other electromagnetic pulses. Energy pours out of the polar regions of the neutron star in intense beams that sweep across the sky. ...
... A pulsar is a rapidly rotating neutron star with a powerful magnetic field that makes it a source of periodic radio and other electromagnetic pulses. Energy pours out of the polar regions of the neutron star in intense beams that sweep across the sky. ...
1 Do Massive Stars Trigger New Waves of Star Formation
... the night sky, and we also orbit the most famous star, our Sun. However, the mechanisms that lead to their formation are still very much unknown. Astronomers also now believe that stars were the first large objects to form in the early universe. Understanding the origins of stars, and thereby the or ...
... the night sky, and we also orbit the most famous star, our Sun. However, the mechanisms that lead to their formation are still very much unknown. Astronomers also now believe that stars were the first large objects to form in the early universe. Understanding the origins of stars, and thereby the or ...
2014 State Test
... D6. (2 pts) The measured parallax of this star is 1.26 milliarcseconds. What is the distance to this star in parsecs? Give your answer to three significant figures. D7. (2 pts) What is the distance modulus associated with the distance you calculated in D6? If you didn’t get an answer to D6 or don’t ...
... D6. (2 pts) The measured parallax of this star is 1.26 milliarcseconds. What is the distance to this star in parsecs? Give your answer to three significant figures. D7. (2 pts) What is the distance modulus associated with the distance you calculated in D6? If you didn’t get an answer to D6 or don’t ...
Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1
... 12-31. The time for a fluctuation in brightness of a quasar allows astronomers to place an upper limit on its a) luminosity. b) size. X c) age. d) distance. Chapter 12 Thought/Writing Questions 12-32. Why are the spiral arms of our Galaxy brighter than the regions between them? The O and B stars for ...
... 12-31. The time for a fluctuation in brightness of a quasar allows astronomers to place an upper limit on its a) luminosity. b) size. X c) age. d) distance. Chapter 12 Thought/Writing Questions 12-32. Why are the spiral arms of our Galaxy brighter than the regions between them? The O and B stars for ...
The Solar System and Beyond
... Distances between planets are very large but they are insignificant compared with distances between stars. Because units that are commonly used to measure distances on Earth such as miles or kilometers are too small for use in astronomy, other units of distance are needed. Within the solar system, t ...
... Distances between planets are very large but they are insignificant compared with distances between stars. Because units that are commonly used to measure distances on Earth such as miles or kilometers are too small for use in astronomy, other units of distance are needed. Within the solar system, t ...
12 The Milky Way - Journigan-wiki
... than open clusters. Their populations can range from a few hundred thousand stars to several million per cluster. Their radii usually range form 40 to 160 light-years. Because they are more massive, they pull their stars into a tighter ball. Astronomers estimate that between 150 to 200 globular clus ...
... than open clusters. Their populations can range from a few hundred thousand stars to several million per cluster. Their radii usually range form 40 to 160 light-years. Because they are more massive, they pull their stars into a tighter ball. Astronomers estimate that between 150 to 200 globular clus ...
Lecture Eight (Powerpoint format) - Flash
... three years on the Hubble Space Telescope. The image covers roughly 1000 AU. The outflow appears to be highly sporadic, but it remains unclear how it is being powered or even which binary member is powering it. ...
... three years on the Hubble Space Telescope. The image covers roughly 1000 AU. The outflow appears to be highly sporadic, but it remains unclear how it is being powered or even which binary member is powering it. ...
Supernovae Gamma-Ray Bursts and and some of their uses
... freshly synthesized heavy elements, and forms what is called a supernova remnant • Supernova remnants may be observed for hundreds of thousands of years as often beautiful, visual objects, but also as emitters of radio waves and X-rays • Close to 150 supernova remnants have been detected in the Milk ...
... freshly synthesized heavy elements, and forms what is called a supernova remnant • Supernova remnants may be observed for hundreds of thousands of years as often beautiful, visual objects, but also as emitters of radio waves and X-rays • Close to 150 supernova remnants have been detected in the Milk ...
Name
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
... 30) The helium fusion process that will occur in the lifetime of a Star with a mass similar to the Sun converts … A) four helium nuclei into one carbon nucleus plus energy B) four helium nuclei into two carbon nucleus plus energy C) two helium nuclei into one carbon nucleus plus energy D) two helium ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.