AmiraPoster3
... shift in line centre may vary significantly. • In this study we only used the helium lines for cross-correlation, so these effects can be ignored. • To correct for the heating effects we ran models using the sophisticated light-curve synthesis program LIGHT2 (Hill 1988). • The program generates non- ...
... shift in line centre may vary significantly. • In this study we only used the helium lines for cross-correlation, so these effects can be ignored. • To correct for the heating effects we ran models using the sophisticated light-curve synthesis program LIGHT2 (Hill 1988). • The program generates non- ...
Lecture 09
... • A transit is when a planet crosses in front of a star. • The resulting eclipse reduces the star’s apparent brightness and tells us the planet’s radius. • The duration of the dip tells us the radius of the star. • The duration of the downward\upward slopes tell us the radius of the planet. • The pl ...
... • A transit is when a planet crosses in front of a star. • The resulting eclipse reduces the star’s apparent brightness and tells us the planet’s radius. • The duration of the dip tells us the radius of the star. • The duration of the downward\upward slopes tell us the radius of the planet. • The pl ...
Lecture Eight (Powerpoint format) - Flash
... Manufactured lenses for Naval Observatory (where Pluto’s moon Charon was discovered) and the University of Chicago Yerkes Observatory (which just shut down research very recently). In 1862, when testing a new 18 inch telescope at the Dearborn observatory at Northwestern University in Evanston, h ...
... Manufactured lenses for Naval Observatory (where Pluto’s moon Charon was discovered) and the University of Chicago Yerkes Observatory (which just shut down research very recently). In 1862, when testing a new 18 inch telescope at the Dearborn observatory at Northwestern University in Evanston, h ...
V - ESO
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
Stellar Evolution
... sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
... sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
1 2 3 4 5 6 Orbital Distance (AU) Orbital Period (Years) 1 2 3 4 5 6 7
... This portion of the homework investigates the relationship between how long it takes a planet to orbit a star (orbital period) and how far away that planet is from the star (orbital distance). We will start by investigating an imaginary planetary system that has an average star like the Sun at the c ...
... This portion of the homework investigates the relationship between how long it takes a planet to orbit a star (orbital period) and how far away that planet is from the star (orbital distance). We will start by investigating an imaginary planetary system that has an average star like the Sun at the c ...
Lecture02-ASTA01 - University of Toronto
... through a layer of air only about 100 kilometres deep (10 km most of it!) • Beyond that, space is nearly empty – with the planets of our solar system several AU away and the far more distant stars scattered many lightyears apart. ...
... through a layer of air only about 100 kilometres deep (10 km most of it!) • Beyond that, space is nearly empty – with the planets of our solar system several AU away and the far more distant stars scattered many lightyears apart. ...
Magnitude Scale
... • Measure of the brightness of a star as seen from the Earth (equivalent of apparent brightness). • Denoted by m • The smaller the number, the brighter the star –m=0 –m=6 ...
... • Measure of the brightness of a star as seen from the Earth (equivalent of apparent brightness). • Denoted by m • The smaller the number, the brighter the star –m=0 –m=6 ...
4-6 Script
... The stars in the Pleiades are hard to miss despite the small space they occupy in the night sky (together, they kind of look like a short-handled little dipper). They shine so bright and vivid that cultures the world over have adopted them into their culture. Try to imagine some of the age old shape ...
... The stars in the Pleiades are hard to miss despite the small space they occupy in the night sky (together, they kind of look like a short-handled little dipper). They shine so bright and vivid that cultures the world over have adopted them into their culture. Try to imagine some of the age old shape ...
October 2014 - Hermanus Astronomy
... equally likely to have a companion star, or do companion stars affect the formation of planets? A team of astronomers, led by Elliott Horch of Southern Connecticut State University, has shown that stars with exoplanets are just as likely to have a binary companion - that is, 40-50% of the host stars ...
... equally likely to have a companion star, or do companion stars affect the formation of planets? A team of astronomers, led by Elliott Horch of Southern Connecticut State University, has shown that stars with exoplanets are just as likely to have a binary companion - that is, 40-50% of the host stars ...
20 Stars/Distances/Magnitudes
... Blink your eyes back and forth. What do you see? What happens to your thumb? Now, extend your thumb out as far as you can. Blink your eyes back and forth again. Now what do you ...
... Blink your eyes back and forth. What do you see? What happens to your thumb? Now, extend your thumb out as far as you can. Blink your eyes back and forth again. Now what do you ...
PHYSICS 113 Practice Questions #2
... b. as the star is dying, a considerable part of its mass will be lost into space c. after the main sequence stage, there is no further fusion of hydrogen anywhere in the star d. at the end of its life, the star will explode as a supernova e. the core of this star will be too massive to form a white ...
... b. as the star is dying, a considerable part of its mass will be lost into space c. after the main sequence stage, there is no further fusion of hydrogen anywhere in the star d. at the end of its life, the star will explode as a supernova e. the core of this star will be too massive to form a white ...
Issue 118 - Apr 2014
... Mira Stars - These long period variables are very large red pulsating stars having brightness magnitude ranges of up to 11 magnitudes and a time period from 24 days to 5.7 years. These stars can be regular, semiregular, or irregular. Some examples are Mira 2.0 - 9.3 (332 day period), R Leo 5.9 - 10. ...
... Mira Stars - These long period variables are very large red pulsating stars having brightness magnitude ranges of up to 11 magnitudes and a time period from 24 days to 5.7 years. These stars can be regular, semiregular, or irregular. Some examples are Mira 2.0 - 9.3 (332 day period), R Leo 5.9 - 10. ...
The star is born
... The proto-star-phase. Protostars are still in the process of attaining star-like structure. Protostars are accompanied by strong outflows and jets, and are surrounded by accretion disks. The disk is pouring more mass onto the protostar. The protostar is hidden within the cocoon of the birth cloud an ...
... The proto-star-phase. Protostars are still in the process of attaining star-like structure. Protostars are accompanied by strong outflows and jets, and are surrounded by accretion disks. The disk is pouring more mass onto the protostar. The protostar is hidden within the cocoon of the birth cloud an ...
Galaxy
... star it is called an eclipsing star Astronomers know there are actually 2 stars by looking at the effects of gravity Our solar system is not the only solar system with planets revolving around a star In 2000, astronomers discovered a solar system about 10.5 light-years away with planets simila ...
... star it is called an eclipsing star Astronomers know there are actually 2 stars by looking at the effects of gravity Our solar system is not the only solar system with planets revolving around a star In 2000, astronomers discovered a solar system about 10.5 light-years away with planets simila ...
Final Exam, Dec. 19, 2015 - Physics@Brock
... (a) About 1%. (b) About 10%. (c) About 50%. (d) [None of the above.] 5. The spectroscopic parallax is a method of determining (a) a star’s chemical composition. (b) a star’s temperature. (c) a star’s distance from parallax angle. (d) a star’s distance using H-R diagram. 6. Which of these main sequen ...
... (a) About 1%. (b) About 10%. (c) About 50%. (d) [None of the above.] 5. The spectroscopic parallax is a method of determining (a) a star’s chemical composition. (b) a star’s temperature. (c) a star’s distance from parallax angle. (d) a star’s distance using H-R diagram. 6. Which of these main sequen ...
HOW do astronomers work? How do they ana
... of the moon period is devoted to direct photography, although some spectroscopic work may also be done then-particularly if it is concerned with nebulae. Those interested in spectroscopic work are at the observatory during the light of the moon, for there are no direct photographs to be made, hence ...
... of the moon period is devoted to direct photography, although some spectroscopic work may also be done then-particularly if it is concerned with nebulae. Those interested in spectroscopic work are at the observatory during the light of the moon, for there are no direct photographs to be made, hence ...
Binaries
... We can also use the Stefan-Boltzmann law L = 4 R2 T4. From the amount of light we are receiving, we measure the luminosity, and from the spectral analysis, we measure the color of the star and determine its temperature we can calculate the diameter indirectly. ...
... We can also use the Stefan-Boltzmann law L = 4 R2 T4. From the amount of light we are receiving, we measure the luminosity, and from the spectral analysis, we measure the color of the star and determine its temperature we can calculate the diameter indirectly. ...
Solutions
... (c) No. Refer back to problem 1. Most of the stars in a globular cluster are low-mass main sequence stars who are burning their nuclear fuel slowly enough that they haven’t yet had time to leave the main sequence. In contrast, most of the light is coming from the most luminous stars (which in this ...
... (c) No. Refer back to problem 1. Most of the stars in a globular cluster are low-mass main sequence stars who are burning their nuclear fuel slowly enough that they haven’t yet had time to leave the main sequence. In contrast, most of the light is coming from the most luminous stars (which in this ...
Kepler`s Laws, Newton`s Laws, and the Search for New Planets
... Laws: the discovery of extrasolar planets during the past decade, none of which has been observed directly, but whose existence and orbital parameters have been deduced by detecting and analyzing the motion of the stars that they orbit. Two other considerations make the correct way of treating the s ...
... Laws: the discovery of extrasolar planets during the past decade, none of which has been observed directly, but whose existence and orbital parameters have been deduced by detecting and analyzing the motion of the stars that they orbit. Two other considerations make the correct way of treating the s ...