Part 1 Notes on Stars - Department of Physics and Astronomy
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
Test
... b. According to current models, why would the formation of a Hot Jupiter like 51 Pegasi b disrupt the formation of an Earth-like planet? 10. Which image shows the DSO Barnard 68? a. What type of nebula is Barnard 68? b. The presence of what substance makes the nebula less see-through in the visible ...
... b. According to current models, why would the formation of a Hot Jupiter like 51 Pegasi b disrupt the formation of an Earth-like planet? 10. Which image shows the DSO Barnard 68? a. What type of nebula is Barnard 68? b. The presence of what substance makes the nebula less see-through in the visible ...
Detecting Extra Solar Planets
... Extrasolar planets have also been detected when they transit, or cross in front of their star as seen from the Earth. This is basically like a solar eclipse, only the planets don't cover much of their sun when they cross, so instead of blocking all of the light, they only block some of it. The light ...
... Extrasolar planets have also been detected when they transit, or cross in front of their star as seen from the Earth. This is basically like a solar eclipse, only the planets don't cover much of their sun when they cross, so instead of blocking all of the light, they only block some of it. The light ...
system of seven planets discovered
... and 25 Earth masses, which orbit the star with periods ranging from about 6 to 600 days. The trace of two additional planets is also visible in the data. One would be a Saturn-like planet (with a minimum mass of 65 Earth masses) orbiting in 2200 days. The other would be the least massive exoplanet e ...
... and 25 Earth masses, which orbit the star with periods ranging from about 6 to 600 days. The trace of two additional planets is also visible in the data. One would be a Saturn-like planet (with a minimum mass of 65 Earth masses) orbiting in 2200 days. The other would be the least massive exoplanet e ...
Extrasolar planets
... • Lots of planets (>500!) have been detected, all in the last 10-15 years • For most of these, we don’t know what the planets are made of, but for the few we can tell, they are probably gas planets like Jupiter • At least, until this week …. ...
... • Lots of planets (>500!) have been detected, all in the last 10-15 years • For most of these, we don’t know what the planets are made of, but for the few we can tell, they are probably gas planets like Jupiter • At least, until this week …. ...
ASTR1010_HW06
... Third Law, then they are planets. The trick, of course, is to get rid of most of the star’s light, otherwise you couldn’t see the faint planets. See Figures 6-16 and 6-17 for actual images. There is a fifth method, not mentioned by the book. This is the astrometric method and it is like method #1, b ...
... Third Law, then they are planets. The trick, of course, is to get rid of most of the star’s light, otherwise you couldn’t see the faint planets. See Figures 6-16 and 6-17 for actual images. There is a fifth method, not mentioned by the book. This is the astrometric method and it is like method #1, b ...
Slides from the third lecture
... • The Kepler Mission is optimized for finding habitable planets ( 0.5 to 10 M ) in the HZ ( near 1 AU ) of solar-like stars • Continuously and simultaneously monitor 100,000 dwarf stars using a 1-meter Schmidt telescope: FOV >100 deg2 with 42 CCDs • Photometric precision of < 20 ppm in 6.5 hours on ...
... • The Kepler Mission is optimized for finding habitable planets ( 0.5 to 10 M ) in the HZ ( near 1 AU ) of solar-like stars • Continuously and simultaneously monitor 100,000 dwarf stars using a 1-meter Schmidt telescope: FOV >100 deg2 with 42 CCDs • Photometric precision of < 20 ppm in 6.5 hours on ...
PH709-assn - University of Kent
... is observed to depend on thesemi-major axis of the exoplanet ...
... is observed to depend on thesemi-major axis of the exoplanet ...
The Life CyCLe of STarS - Origins
... together. Astrophysicists calculate that this stable balance between pressure and gravity can last for a very long time (10 billion years for a star like our sun), for as long as the fusion reactions continue. 33 Star Aging. At some point, the fuel for fusion gets used up, like a car running out of ...
... together. Astrophysicists calculate that this stable balance between pressure and gravity can last for a very long time (10 billion years for a star like our sun), for as long as the fusion reactions continue. 33 Star Aging. At some point, the fuel for fusion gets used up, like a car running out of ...
Lecture 34. Extrasolar Planets.
... Observes the wobble in nearby stars against a backdrop of distant stars. Wobble caused by orbiting around the COM. The wobble is extremely small - very difficult to detect. Requires very sensitive instruments and way to diminish atmospheric effects. ...
... Observes the wobble in nearby stars against a backdrop of distant stars. Wobble caused by orbiting around the COM. The wobble is extremely small - very difficult to detect. Requires very sensitive instruments and way to diminish atmospheric effects. ...
AAS.StarFormation - National Optical Astronomy Observatory
... Implications for Planet Building • In combination, these observations suggest: – accretion disks surround all forming stars – disk masses and sizes are similar to our solar system ...
... Implications for Planet Building • In combination, these observations suggest: – accretion disks surround all forming stars – disk masses and sizes are similar to our solar system ...
Lecture22 - Indiana University Astronomy
... More massive, brighter stars have wider HZ. However, massive, bright stars are much more short-lived than smaller, stars. In the case of the massive O stars and B main sequence stars, these very objects race through their life-cycles in only a few tens of millions of years – too quickly to allow ev ...
... More massive, brighter stars have wider HZ. However, massive, bright stars are much more short-lived than smaller, stars. In the case of the massive O stars and B main sequence stars, these very objects race through their life-cycles in only a few tens of millions of years – too quickly to allow ev ...
15 Aug 2009
... light steadily for far longer than our sun's 10-billion year lifetime (of which 5 billion years have now passed). Massachusetts Institute of Technology astronomer Sara Seeger thinks that "infrared astronomy," based on invisible light whose wavelength is a little longer than visible light's wavelengt ...
... light steadily for far longer than our sun's 10-billion year lifetime (of which 5 billion years have now passed). Massachusetts Institute of Technology astronomer Sara Seeger thinks that "infrared astronomy," based on invisible light whose wavelength is a little longer than visible light's wavelengt ...
Hungry Young Stars: A New Explanation for the FU Ori Outbursts
... • We provide an explanation for the origin of FU Ori bursts. • A young star devours embryos that form in the disk, resulting in colossal bursts of luminosity. This process repeats as long as nebular material rains onto the disk. • The new feature in our model is the self-consistent formation and evo ...
... • We provide an explanation for the origin of FU Ori bursts. • A young star devours embryos that form in the disk, resulting in colossal bursts of luminosity. This process repeats as long as nebular material rains onto the disk. • The new feature in our model is the self-consistent formation and evo ...
Supplemental Educational Support Materials
... distant from Earth. They are small and dark, and unlike stars, they do not emit visible light. (They only reflect the visible light of their star.) Therefore, extrasolar planets are faint to see. Imaging a planet is extremely difficult because it gets lost in the glare of its much brighter and large ...
... distant from Earth. They are small and dark, and unlike stars, they do not emit visible light. (They only reflect the visible light of their star.) Therefore, extrasolar planets are faint to see. Imaging a planet is extremely difficult because it gets lost in the glare of its much brighter and large ...
Ramos_Poster
... The study of planet formation mechanisms is a central part of our search for an understanding of the origin of the Earth and Solar System. The motivation to study the environments of planet formation has become more intense since the discovery of the first giant planets around nearby solar-type star ...
... The study of planet formation mechanisms is a central part of our search for an understanding of the origin of the Earth and Solar System. The motivation to study the environments of planet formation has become more intense since the discovery of the first giant planets around nearby solar-type star ...
Extrasolar Planets
... • For young extrasolar planets we could look to the planet’s thermal emission whose contrast ratio is much more favorable, perhaps by as many as four orders of magnitude at 5-10 microns. ...
... • For young extrasolar planets we could look to the planet’s thermal emission whose contrast ratio is much more favorable, perhaps by as many as four orders of magnitude at 5-10 microns. ...
Solutions2
... d) Do you think you might be able to resolve its disk with the U of A telescope? Why or why not (show a calculation)? The U of A telescope has an aperture of 12 inches (0.33 m), and therefore an angular resolution (in V band, 550 nm) of θ = 1.22 ∗ (5.5 × 10−7 m/0.33m) = 2.0 × 10−6 radians, or 0.4”. ...
... d) Do you think you might be able to resolve its disk with the U of A telescope? Why or why not (show a calculation)? The U of A telescope has an aperture of 12 inches (0.33 m), and therefore an angular resolution (in V band, 550 nm) of θ = 1.22 ∗ (5.5 × 10−7 m/0.33m) = 2.0 × 10−6 radians, or 0.4”. ...
Stellar Magnitude, Distance, and Motion
... o The Solar System is about 80 Astronomical Units in diameter. o The nearest star (other than the sun) is 4.3 light years away. o Our Galaxy (the Milky Way) is about 100,000 light years in diameter. o Diameter of local cluster of galaxies: about 1 Megaparsec. o Distance to M87 in the Virgo cluster: ...
... o The Solar System is about 80 Astronomical Units in diameter. o The nearest star (other than the sun) is 4.3 light years away. o Our Galaxy (the Milky Way) is about 100,000 light years in diameter. o Diameter of local cluster of galaxies: about 1 Megaparsec. o Distance to M87 in the Virgo cluster: ...
From Big bang to lives on planets
... Advantages of the Doppler Method –Most successful method –About 85% of known exoplanets are detected by the technique –The Doppler method is sensitive to massive planets around relatively nearby stars Advantages of Transits –Transits offer the only way we currently have to make a direct measuremen ...
... Advantages of the Doppler Method –Most successful method –About 85% of known exoplanets are detected by the technique –The Doppler method is sensitive to massive planets around relatively nearby stars Advantages of Transits –Transits offer the only way we currently have to make a direct measuremen ...
Document
... was not a sine curve, and I wonder if the fact that there is a second star is possibly causing a three body problem, rather than 2 body. This has taken me the better part of two days to go through all the information. The value of the parent star varied in data from .99 up to 1.1 solar masses, and f ...
... was not a sine curve, and I wonder if the fact that there is a second star is possibly causing a three body problem, rather than 2 body. This has taken me the better part of two days to go through all the information. The value of the parent star varied in data from .99 up to 1.1 solar masses, and f ...
Lecture 21
... (e) Now what will be the period of the star's Doppler shift pattern for its spectral lines? (f) What is the orbital speed of the star in its orbit around the center of mass? (g) What will be the wavelength shift for a visible line (say with wavelength 500 nm)? ...
... (e) Now what will be the period of the star's Doppler shift pattern for its spectral lines? (f) What is the orbital speed of the star in its orbit around the center of mass? (g) What will be the wavelength shift for a visible line (say with wavelength 500 nm)? ...
S90 U5 T3 Notes - Cochrane High School
... Don’t forget! Wavelength measures the distance between two high or low points on a wave. Frequency is the measure of how many waves pass in a given time period. ...
... Don’t forget! Wavelength measures the distance between two high or low points on a wave. Frequency is the measure of how many waves pass in a given time period. ...
PLANETS BEYOND OUR SOLAR SYSTEM By William Reville
... be small and rocky, as in our solar system. Only in the outer reaches of the solar system will enough gas, hydrogen and helium, be available to form gassy planets like Jupiter, Saturn, Uranus and Neptune. Astronomers feel certain that only the densest clouds, from which solar systems form, contain e ...
... be small and rocky, as in our solar system. Only in the outer reaches of the solar system will enough gas, hydrogen and helium, be available to form gassy planets like Jupiter, Saturn, Uranus and Neptune. Astronomers feel certain that only the densest clouds, from which solar systems form, contain e ...
Beta Pictoris
Beta Pictoris (β Pic, β Pictoris) is the second brightest star in the constellation Pictor. It is located 63.4 light years from our solar system, and is 1.75 times as massive and 8.7 times as luminous as the Sun. The Beta Pictoris system is very young, only 8–20 million years old, although it is already in the main sequence stage of its evolution. Beta Pictoris is the title member of the Beta Pictoris moving group, an association of young stars which share the same motion through space and have the same age.Beta Pictoris shows an excess of infrared emission compared to normal stars of its type, which is caused by large quantities of dust and gas (including carbon monoxide) near the star. Detailed observations reveal a large disk of dust and gas orbiting the star, which was the first debris disk to be imaged around another star. In addition to the presence of several planetesimal belts and cometary activity, there are indications that planets have formed within this disk and that the processes of planet formation may still be ongoing. Material from the Beta Pictoris debris disk is thought to be the dominant source of interstellar meteoroids in our solar system.The European Southern Observatory (ESO) has confirmed the presence of a planet, Beta Pictoris b, matching previous predictions, through the use of direct imagery, orbiting in the plane of the debris disk surrounding the star. This planet is currently the closest extrasolar planet to its star ever photographed: the observed separation is roughly the same as the distance between Saturn and the Sun.