Topic 3 Assignment - Science 9 Portfolio
... made of. Stars have dark bands in distinct sequences and thicknesses on their spectra. Each element that is present in the star creates its own black-line ‘fingerprint’. The spectra of the star are then compared to known spectra of elements to determine the star’s composition. This is called spectra ...
... made of. Stars have dark bands in distinct sequences and thicknesses on their spectra. Each element that is present in the star creates its own black-line ‘fingerprint’. The spectra of the star are then compared to known spectra of elements to determine the star’s composition. This is called spectra ...
Photometric Surveys and Variable stars
... • gamma Doradus The MSTO of NGC 2301 lies around A0, so delta Scuti and gamma Doradus stars should be present. Perhaps some cluster Cepheids, too? ...
... • gamma Doradus The MSTO of NGC 2301 lies around A0, so delta Scuti and gamma Doradus stars should be present. Perhaps some cluster Cepheids, too? ...
Solution Set
... Even though all large galaxies are though to have supermassive black hole, they need to be accreting material at a high rate to produce an AGN. At any given time, only about 1% of SMBHs wil ...
... Even though all large galaxies are though to have supermassive black hole, they need to be accreting material at a high rate to produce an AGN. At any given time, only about 1% of SMBHs wil ...
Milky Way - Wayne Hu`s Tutorials
... Calibrated locally by moving cluster and other methods • Measure the period of oscillation, infer a luminosity and hence an absolute magnitude, infer a distance from the observed apparent magnitude ...
... Calibrated locally by moving cluster and other methods • Measure the period of oscillation, infer a luminosity and hence an absolute magnitude, infer a distance from the observed apparent magnitude ...
Oct 06, 2001
... 9. Which of the stars listed above has the longest remaining lifetime? 10. Which of the stars listed above has a spectral type different from its original spectral type? ...
... 9. Which of the stars listed above has the longest remaining lifetime? 10. Which of the stars listed above has a spectral type different from its original spectral type? ...
Student Worksheet - Indiana University Astronomy
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
... young star cluster near its center. The dust lanes appear dark because they obscure visible light, and are thus seen in silhouette against the brighter, glowing, hydrogen gas. Surrounding the red nebula is a blue reflection nebula, especially bright at northern end. The reflection nebula glows by re ...
Origin of the Elements and their Isotopes
... • Protons are positively charged, neutrons are neutral and electrons are negatively charged. ...
... • Protons are positively charged, neutrons are neutral and electrons are negatively charged. ...
observingnebulaeclusters-1
... Space Telescope Science Institute. It begins with a "backyard" view of the sky around the constellation Orion (by Skip Westphal, STScI) and a more detailed view of the Orion Nebula, M42 . Images taken with the 4-meter telescope at Kitt Peak National Observatory. A spectacular cloud of gas surrounds ...
... Space Telescope Science Institute. It begins with a "backyard" view of the sky around the constellation Orion (by Skip Westphal, STScI) and a more detailed view of the Orion Nebula, M42 . Images taken with the 4-meter telescope at Kitt Peak National Observatory. A spectacular cloud of gas surrounds ...
–1– 1. The Luminosity of Protostars We derived in the previous
... Imagine a star with a radius R⋆ and temperature T⋆ surrounded by an optically thick shell of dust at a radius Rshell . Assuming that the shell is in temperature equilibrium, i.e. it is emitting as much power as it is absorbing, then. Lshell = L⋆ ...
... Imagine a star with a radius R⋆ and temperature T⋆ surrounded by an optically thick shell of dust at a radius Rshell . Assuming that the shell is in temperature equilibrium, i.e. it is emitting as much power as it is absorbing, then. Lshell = L⋆ ...
AST 101 INTRODUCTION TO ASTRONOMY SPRING 2008
... E 7. Which of the following statements about the future fate of our Sun is FALSE? A. The Sun will burn helium into carbon, but never get hot enough its core to burn carbon into oxygen B. When the Sun exhausts all hydrogen in its core it will leave the main sequence C. At the end of its life, all tha ...
... E 7. Which of the following statements about the future fate of our Sun is FALSE? A. The Sun will burn helium into carbon, but never get hot enough its core to burn carbon into oxygen B. When the Sun exhausts all hydrogen in its core it will leave the main sequence C. At the end of its life, all tha ...
Homework 4 - UCLA Astronomy
... Due: Friday, May 9, 2008 in class or to Ian by noon. Reading: Chapter on The Milky Way Problems: ...
... Due: Friday, May 9, 2008 in class or to Ian by noon. Reading: Chapter on The Milky Way Problems: ...
Epsilon Aurigae Mystery and Opportunity
... • A 3-day workshop, focused on observing and education/public outreach, will be held at the Adler Planetarium in Chicago, August 5-7, 2009. The workshop will occur just days before the eclipse of epsilon Aurigae is predicted to begin. • Video of talks at the workshops will be placed ...
... • A 3-day workshop, focused on observing and education/public outreach, will be held at the Adler Planetarium in Chicago, August 5-7, 2009. The workshop will occur just days before the eclipse of epsilon Aurigae is predicted to begin. • Video of talks at the workshops will be placed ...
Module Outlines
... Today, the magnitude system has been extended to include much fainter and brighter objects. ...
... Today, the magnitude system has been extended to include much fainter and brighter objects. ...
Chapter 12
... – Superimposed on this orbital motion are small random motions of about 20 km/sec – In addition to their motion through space, stars spin on their axes and this spin can be measured using the Doppler shift technique – young stars are found to rotate faster than old stars ...
... – Superimposed on this orbital motion are small random motions of about 20 km/sec – In addition to their motion through space, stars spin on their axes and this spin can be measured using the Doppler shift technique – young stars are found to rotate faster than old stars ...
GRB Progenitors and their environments
... • Helium-merger models (the merger of a star with a compact object – who named these?): inspiral of compact object both ejects outer layers and spins up the soon-to-be accreting material. • Environments surrounding both models tightly tied to stellar winds/binary mass ejection. ...
... • Helium-merger models (the merger of a star with a compact object – who named these?): inspiral of compact object both ejects outer layers and spins up the soon-to-be accreting material. • Environments surrounding both models tightly tied to stellar winds/binary mass ejection. ...
m 1
... 1. Use stars < 100pc to calibrate MV for spectral classes 2. For unknown star: a) use CCD to measure mV b) use spectrograph to find spectral class c) use calibration from (1) to get MV d) use distance modulus to calculate d ...
... 1. Use stars < 100pc to calibrate MV for spectral classes 2. For unknown star: a) use CCD to measure mV b) use spectrograph to find spectral class c) use calibration from (1) to get MV d) use distance modulus to calculate d ...
1704 chart front - Adventure Science Center
... Maiden. Neither of these constellations has any other bright stars. Even under dark skies away from city lights, it’s hard to imagine these mythological figures just by connecting the dots. Not too far from Spica is the bright planet Jupiter. If you have binoculars, you may be able to see the giant p ...
... Maiden. Neither of these constellations has any other bright stars. Even under dark skies away from city lights, it’s hard to imagine these mythological figures just by connecting the dots. Not too far from Spica is the bright planet Jupiter. If you have binoculars, you may be able to see the giant p ...
Discussion Activity #9
... C. There is a balance within the Sun between the outward push of pressure and the inward pull of gravity. D. The Sun always has the same amount of mass, creating the same gravitational force. 2. Which of the following correctly describes how the process of gravitational contraction can ...
... C. There is a balance within the Sun between the outward push of pressure and the inward pull of gravity. D. The Sun always has the same amount of mass, creating the same gravitational force. 2. Which of the following correctly describes how the process of gravitational contraction can ...
Part 3
... the less massive component (secondary star) be covered， the effective temperature of the secondary star is higher, its spectral type always to be G-K). ...
... the less massive component (secondary star) be covered， the effective temperature of the secondary star is higher, its spectral type always to be G-K). ...
15-1 Notes - westscidept
... 15-1 Notes: Stars Scientists know that the _______ of star indicates the star’s temperature. _____ stars are the coolest, and _______ stars are the hottest. When you look at white light through a prism, you see a rainbow of colors called a ___________. Astronomers use a ________________ to separate ...
... 15-1 Notes: Stars Scientists know that the _______ of star indicates the star’s temperature. _____ stars are the coolest, and _______ stars are the hottest. When you look at white light through a prism, you see a rainbow of colors called a ___________. Astronomers use a ________________ to separate ...
Cepheid variable stars
... Virginis and RR Lyrae stars are giant stars of different masses that are evolving through the appropriate temperature range. ...
... Virginis and RR Lyrae stars are giant stars of different masses that are evolving through the appropriate temperature range. ...
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.