Stellar Winds and Mass Loss
... CO J=1→0 lines are typically used The velocities at this range are much lower than the escape speed of the star, but they still indicate mass loss Knapp and Morris derived an expression for the CO mass loss rate in 1985 ...
... CO J=1→0 lines are typically used The velocities at this range are much lower than the escape speed of the star, but they still indicate mass loss Knapp and Morris derived an expression for the CO mass loss rate in 1985 ...
Constants and Equations
... T☉ 5.8103 K M☉ 2.01030 kg G (Gravitational Constant) 6.6710-11m3kg-1s-2 (Stephan-Boltzmann Constant) 5.6710-8 Wm-2K-4 c (Speed of Light in Vacuum) 3108 ms-1 ...
... T☉ 5.8103 K M☉ 2.01030 kg G (Gravitational Constant) 6.6710-11m3kg-1s-2 (Stephan-Boltzmann Constant) 5.6710-8 Wm-2K-4 c (Speed of Light in Vacuum) 3108 ms-1 ...
w 2012-01-13 Stellar Life Cycle
... Planetary nebulae are shells of gas thrown out by some stars near the end of their lives. Our Sun will probably produce a planetary nebula in about 5 billion years. They have nothing at all to do with planets; the terminology was invented because they often look a little like planets in small telesc ...
... Planetary nebulae are shells of gas thrown out by some stars near the end of their lives. Our Sun will probably produce a planetary nebula in about 5 billion years. They have nothing at all to do with planets; the terminology was invented because they often look a little like planets in small telesc ...
Milky Way galaxy drawing
... Name ______________________________________________________ Date______________________________ Hour__________ Rubric for Milky Way Galaxy Drawing 4 points ...
... Name ______________________________________________________ Date______________________________ Hour__________ Rubric for Milky Way Galaxy Drawing 4 points ...
Project Packet - Montville.net
... 4. If your star is a II, default to the chart for III stars. b. V is the luminosity class 1. To determine star luminosity class, go to this link: Star Classification System. http://www.enchantedlearning.com/subjects/astronomy/stars/startypes.shtml 2. Scroll down to the Yerkes luminosity classes tabl ...
... 4. If your star is a II, default to the chart for III stars. b. V is the luminosity class 1. To determine star luminosity class, go to this link: Star Classification System. http://www.enchantedlearning.com/subjects/astronomy/stars/startypes.shtml 2. Scroll down to the Yerkes luminosity classes tabl ...
The Interstellar Medium Chapter 10
... invisible. The thin gas and dust that drifts through space between the stars is produced in part by dying stars and can give birth to new stars. This chapter will show you how important spectroscopic analysis is in astronomy and will help you answer three essential questions: • How do visual-wavelen ...
... invisible. The thin gas and dust that drifts through space between the stars is produced in part by dying stars and can give birth to new stars. This chapter will show you how important spectroscopic analysis is in astronomy and will help you answer three essential questions: • How do visual-wavelen ...
E1 Introduction to the universe
... An open Universe is one that continues to expand forever. The force of gravity slows the rate of recession of the galaxies down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses ba ...
... An open Universe is one that continues to expand forever. The force of gravity slows the rate of recession of the galaxies down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses ba ...
s-process
... The Galaxy in time – a brief review of the formation of the Milky Way and its structural components The origin of the elements – back to B2FH! A stroll through the Periodic Table A timeline of Galactic chemical enrichment What does it all mean? ...
... The Galaxy in time – a brief review of the formation of the Milky Way and its structural components The origin of the elements – back to B2FH! A stroll through the Periodic Table A timeline of Galactic chemical enrichment What does it all mean? ...
Lec09_ch11_lifecycleofstars
... • An H-R census of the Globular cluster stars reveals the age of the cluster – since the globular cluster stars are gravitationally bound close together, they are the same distance from us • use apparent magnitude ...
... • An H-R census of the Globular cluster stars reveals the age of the cluster – since the globular cluster stars are gravitationally bound close together, they are the same distance from us • use apparent magnitude ...
Earth and Stars
... shadow cast by a gnomon at Alexandria. He found a value of 1/50th of a circumference (i.e. 7.12°) and derived the value of the terrestrial circumference: 50 x 5.000 = 250.000 stadia. Although our idea of the exact value of the stadium (which was not the same at Athens, Alexandria or Rome) is fairly ...
... shadow cast by a gnomon at Alexandria. He found a value of 1/50th of a circumference (i.e. 7.12°) and derived the value of the terrestrial circumference: 50 x 5.000 = 250.000 stadia. Although our idea of the exact value of the stadium (which was not the same at Athens, Alexandria or Rome) is fairly ...
types of stars, luminosity, and brightness
... star. 5. The absolute brightness is the brightness that would be measured at a standard distance of 10 pc. Apparent brightness is the brightness of a star measured from Earth. 6. Absolute brightness is the luminosity of a star as it would be measured at 10 pc. Luminosity is the intrinsic energy per ...
... star. 5. The absolute brightness is the brightness that would be measured at a standard distance of 10 pc. Apparent brightness is the brightness of a star measured from Earth. 6. Absolute brightness is the luminosity of a star as it would be measured at 10 pc. Luminosity is the intrinsic energy per ...
Summer Triangle (Winter in the south hemisphere) Lyra
... Cygnus is one of the major constellations in the northern hemisphere's summer sky, best seen from June through November. It is also known as the Northern Cross. History and Mythology Cygnus has been associated with several myths. One myth represents the bird into which Zeus transformed himself to s ...
... Cygnus is one of the major constellations in the northern hemisphere's summer sky, best seen from June through November. It is also known as the Northern Cross. History and Mythology Cygnus has been associated with several myths. One myth represents the bird into which Zeus transformed himself to s ...
Measuring Motion, Doppler Effect—28 Oct Outline • Announcements
... – Separation of two wavelengths grows larger, then smaller. ...
... – Separation of two wavelengths grows larger, then smaller. ...
Stages - A Summary - University of Dayton
... outward luminosity and inward gravity. Our star has reached the Zero Age Main Sequence, where it will stay for over 90% of its life, virtually unchanged externally. [Note : Stars of different masses experience similar evolutionary tracks on the H-R Diagram, but end up at different points on the ZAMS ...
... outward luminosity and inward gravity. Our star has reached the Zero Age Main Sequence, where it will stay for over 90% of its life, virtually unchanged externally. [Note : Stars of different masses experience similar evolutionary tracks on the H-R Diagram, but end up at different points on the ZAMS ...
Life Cycle of Stars
... Hubble Space Telescope ACS/HRC – NASA, ESA, N.Evans (Harvard-Smithsonian CfA), and H.Bond (S TScl) ...
... Hubble Space Telescope ACS/HRC – NASA, ESA, N.Evans (Harvard-Smithsonian CfA), and H.Bond (S TScl) ...
HighRedshiftGalaxies
... H flux arises from recombination photons linked to those emitted below the Lyman limit from main 6 years. sequence stars with lifetimes 10 ...
... H flux arises from recombination photons linked to those emitted below the Lyman limit from main 6 years. sequence stars with lifetimes 10 ...
Stars III - Indiana University Astronomy
... • Sun-like stars with <2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs • Intermediate mass stars can make elements heavier than carbon but end as white dwarfs ...
... • Sun-like stars with <2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs • Intermediate mass stars can make elements heavier than carbon but end as white dwarfs ...
Educator Guide: Starlab (Grades 6-8)
... and its outer layers cool and take on a reddish hue. Red Supergiant – an especially large red giant star. Red supergiant stars can have dimeters greater than 500 times that of the Sun. Betelgeuse in the constellation Orion and Antares in Scorpius are red supergiant stars. Rotation – spinning on a ...
... and its outer layers cool and take on a reddish hue. Red Supergiant – an especially large red giant star. Red supergiant stars can have dimeters greater than 500 times that of the Sun. Betelgeuse in the constellation Orion and Antares in Scorpius are red supergiant stars. Rotation – spinning on a ...
Classifying the Spectra of Stars:
... numbered 0 to 9. A star midway through the range between F0 and G0 would be an F5 type star. The Sun is a G2 type star. In addition to subtypes, there is also a luminosity class, designated by roman numerals from I to V. Class V stars are main sequence stars (which we will study later) and are the o ...
... numbered 0 to 9. A star midway through the range between F0 and G0 would be an F5 type star. The Sun is a G2 type star. In addition to subtypes, there is also a luminosity class, designated by roman numerals from I to V. Class V stars are main sequence stars (which we will study later) and are the o ...
Rogava_Course_-_First_lecture
... impact on each other, stars essentially evolve separately. • Semidetached binary stars: one of the components fills its Roche lobe and the other does not. Gas from the surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evo ...
... impact on each other, stars essentially evolve separately. • Semidetached binary stars: one of the components fills its Roche lobe and the other does not. Gas from the surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evo ...
The Luminosity
... Massive stars die and turn into black holes. • After some massive stars (> 10 suns) explode as supernovae, they will retain a mass of 2 to 3 solar masses in their cores. • Nothing in the universe is strong enough to hold up the remaining mass against the force of gravity, so it collapses into a b ...
... Massive stars die and turn into black holes. • After some massive stars (> 10 suns) explode as supernovae, they will retain a mass of 2 to 3 solar masses in their cores. • Nothing in the universe is strong enough to hold up the remaining mass against the force of gravity, so it collapses into a b ...
The Constellations
... Summary—Movements of Stars Pattern in the Sky • Star pattern repeats itself about every 24 hours… because of the rotation of Earth with respect to the distant stars! • Star pattern in the winter is different from that in the summer… because of the revolution of Earth around the Sun! • Stars do move ...
... Summary—Movements of Stars Pattern in the Sky • Star pattern repeats itself about every 24 hours… because of the rotation of Earth with respect to the distant stars! • Star pattern in the winter is different from that in the summer… because of the revolution of Earth around the Sun! • Stars do move ...
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.