Exam 3 Study Guide
... Questions you can answer to study. See if you can write your own multiple choice question for these topics! What are three properties that distinguish elliptical galaxies from spiral galaxies? How do spiral galaxies form? How do elliptical galaxies form? Where in a spiral galaxy might you find star ...
... Questions you can answer to study. See if you can write your own multiple choice question for these topics! What are three properties that distinguish elliptical galaxies from spiral galaxies? How do spiral galaxies form? How do elliptical galaxies form? Where in a spiral galaxy might you find star ...
Exploration of the Milky Way and Nearby galaxies
... Extremely metal-poor stars in the Milky Way and the Local group ...
... Extremely metal-poor stars in the Milky Way and the Local group ...
STARS Chapter 8 Section 1
... • Parallax is the object’s apparent shift in motion when viewed from different locations. It is an optical effect. • Astronomers can measure parallax and use it to calculate exact distances to stars. • Does the man on the right(V2) see the moon as closer or farther away than the man on the left? • W ...
... • Parallax is the object’s apparent shift in motion when viewed from different locations. It is an optical effect. • Astronomers can measure parallax and use it to calculate exact distances to stars. • Does the man on the right(V2) see the moon as closer or farther away than the man on the left? • W ...
Virtual HR Diagram Lab
... 8. Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating-alternately growing bigger and smaller- ...
... 8. Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating-alternately growing bigger and smaller- ...
Answers for the HST Scavenger Hunt
... Give a definition of these kinds of stars. Hot, dense remains of a low-mass star like our Sun that has exhausted its sources of fuel for thermonuclear fusion. What is a Wolf-Rayet Star? Massive stars, which are usually are surrounded by outflowing gas clouds. How is this star type different from whi ...
... Give a definition of these kinds of stars. Hot, dense remains of a low-mass star like our Sun that has exhausted its sources of fuel for thermonuclear fusion. What is a Wolf-Rayet Star? Massive stars, which are usually are surrounded by outflowing gas clouds. How is this star type different from whi ...
Review Questions for Chp 2
... 77. In summer in Doylestown what kind of rays from the sun are we receiving? ...
... 77. In summer in Doylestown what kind of rays from the sun are we receiving? ...
Star Birth: The Formation of Stars Jonathan Rowles
... A star is a luminous ball of gas. They produce energy by the nuclear fusion of hydrogen to form helium. They range in size from 0.08 times the mass of the Sun to up to 120 Solar masses. They can have lifetimes ranging from a few million years to the age of the universe. ...
... A star is a luminous ball of gas. They produce energy by the nuclear fusion of hydrogen to form helium. They range in size from 0.08 times the mass of the Sun to up to 120 Solar masses. They can have lifetimes ranging from a few million years to the age of the universe. ...
Wavelength
... outer portion expands • Eventually, the outer parts grow larger and drift out into space creating a planetary nebula. ...
... outer portion expands • Eventually, the outer parts grow larger and drift out into space creating a planetary nebula. ...
No Slide Title
... • For example, if our sun was the dot over this “i”, the nearest star would be ten miles away ...
... • For example, if our sun was the dot over this “i”, the nearest star would be ten miles away ...
Properties of Stars
... would be easier and more helpful, since we know a lot about the Sun and it is a star. Let’s get rid of the constants ! ...
... would be easier and more helpful, since we know a lot about the Sun and it is a star. Let’s get rid of the constants ! ...
Stars Study Guide KEY
... Galaxies are still moving outward from the explosion (and away from each other). Cosmic background radiation has been discovered- it is supposed to be heat left over from the explosion. 19. Describe how galaxies are moving in the universe at this time. Galaxies are moving away from each other. They ...
... Galaxies are still moving outward from the explosion (and away from each other). Cosmic background radiation has been discovered- it is supposed to be heat left over from the explosion. 19. Describe how galaxies are moving in the universe at this time. Galaxies are moving away from each other. They ...
Astronomy 1 – Winter 2011
... The Inverse-Square Law Radiation from a light source illuminates an area that increases as the square of the distance from the source. The apparent brightness decreases as the square of the distance. The brightness at d = 2 is 1/(22) = 1/4 of the brightness at d = 1, and the brightness at d = 3 is ...
... The Inverse-Square Law Radiation from a light source illuminates an area that increases as the square of the distance from the source. The apparent brightness decreases as the square of the distance. The brightness at d = 2 is 1/(22) = 1/4 of the brightness at d = 1, and the brightness at d = 3 is ...
TYPES OF STARS
... the locations (energies) at which absorption or emission lines occur can be used to “fingerprint” the star’s composition. The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines ( ...
... the locations (energies) at which absorption or emission lines occur can be used to “fingerprint” the star’s composition. The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines ( ...
HW #4 (due March 27)
... the locations (energies) at which absorption or emission lines occur can be used to “fingerprint” the star’s composition. The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines ( ...
... the locations (energies) at which absorption or emission lines occur can be used to “fingerprint” the star’s composition. The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines ( ...
Chapter 21 notes - Clinton Public Schools
... Neutron stars: after supergiant explodes, material may form neutron star. Smaller and denser than white dwarfs: can contain 3X mass as the sun. Neutron stars can also be called pulsars because the rapidly spinning neutron star is spinning hundreds of times per second, sending pulsating radio waves: ...
... Neutron stars: after supergiant explodes, material may form neutron star. Smaller and denser than white dwarfs: can contain 3X mass as the sun. Neutron stars can also be called pulsars because the rapidly spinning neutron star is spinning hundreds of times per second, sending pulsating radio waves: ...
Masses are much harder than distance, luminosity, or temperature
... • Range of different mass stars! ...
... • Range of different mass stars! ...
Blowing Bubbles in Space: The Birth and Death of Practically
... • Planetary nebulae are the final stages in the lives of low-mass stars, such as our Sun. As they reach the ends of their lives, their late RGB superwinds send off large amounts of material into space. Although the nebulae can look like a fireworks display, the process of developing a nebula is (usu ...
... • Planetary nebulae are the final stages in the lives of low-mass stars, such as our Sun. As they reach the ends of their lives, their late RGB superwinds send off large amounts of material into space. Although the nebulae can look like a fireworks display, the process of developing a nebula is (usu ...
Bang To Sol - Transcript
... natural to wonder what could provide such awesome energies? (Black Holes…) (spoken with an echo) ...
... natural to wonder what could provide such awesome energies? (Black Holes…) (spoken with an echo) ...
Supernovae: Heavy Elements
... • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ejected back into space in a c ...
... • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ejected back into space in a c ...
Stellar Metamorphosis: The Nearest Star
... Abstract: In stellar metamorphosis humanities’ closest star is the Earth itself. Explanation is provided. In the so-called “established sciences” the closest star to the Earth is the Sun, and the closest star to Earth besides the Sun is Proxima Centauri. This is not complete. According to stellar me ...
... Abstract: In stellar metamorphosis humanities’ closest star is the Earth itself. Explanation is provided. In the so-called “established sciences” the closest star to the Earth is the Sun, and the closest star to Earth besides the Sun is Proxima Centauri. This is not complete. According to stellar me ...
Lecture Ten - The Sun Amongst the Stars Part II
... O-type stars have very few lines because they are so hot that most of their elements have been stripped of electrons – while in cooler, M-type stars, far more atoms retain their electrons. Patterns of absorption lines can reveal the temperatures of the stars to a precision within 50 degrees K – a f ...
... O-type stars have very few lines because they are so hot that most of their elements have been stripped of electrons – while in cooler, M-type stars, far more atoms retain their electrons. Patterns of absorption lines can reveal the temperatures of the stars to a precision within 50 degrees K – a f ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.