Observational Constraints The Nebular Hypothesis
... 2. The mass of the giant planets decreases with orbital distance. 3. Heavy element enrichment increases with decreasing mass. Outside of the Solar System: 1. While there are many observed extrasolar giant planets, they still appear to be less common than small (terrestrial) planets. An up-to-date ca ...
... 2. The mass of the giant planets decreases with orbital distance. 3. Heavy element enrichment increases with decreasing mass. Outside of the Solar System: 1. While there are many observed extrasolar giant planets, they still appear to be less common than small (terrestrial) planets. An up-to-date ca ...
The Mt John University Observatory search for Earth
... Abstract: The ‘holy grail’ in planet hunting is the detection of an Earth-analogue: a planet with similar mass as the Earth and an orbit inside the habitable zone. If we can find such an Earth-analogue around one of the stars in the immediate solar neighbourhood, we could potentially even study it in ...
... Abstract: The ‘holy grail’ in planet hunting is the detection of an Earth-analogue: a planet with similar mass as the Earth and an orbit inside the habitable zone. If we can find such an Earth-analogue around one of the stars in the immediate solar neighbourhood, we could potentially even study it in ...
Chapter 7
... formed Sun (protosun) will prevent the condensation of more volatile elements. Planets forming there will thus be made of nonvolatile, dense material. 4. Farther out, the eddies are larger and the temperatures cooler so large planets can form that are composed of volatile elements (light gases). 5. ...
... formed Sun (protosun) will prevent the condensation of more volatile elements. Planets forming there will thus be made of nonvolatile, dense material. 4. Farther out, the eddies are larger and the temperatures cooler so large planets can form that are composed of volatile elements (light gases). 5. ...
ph709-15-testrevision
... Direct imaging of planets is difficult because of the enormous difference in brightness between the star and the planet, and the small angular separation between them. Direct detection: must be large and distant from star Circumstellar dust discs. (Circumstantial evidence.) Disc of material around t ...
... Direct imaging of planets is difficult because of the enormous difference in brightness between the star and the planet, and the small angular separation between them. Direct detection: must be large and distant from star Circumstellar dust discs. (Circumstantial evidence.) Disc of material around t ...
15.6 Planets Beyond the Solar System
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
The Origin of the Solar System and Other Planetary Systems
... The Role of Catastrophes Condensation-accretion theory explains the 10 properties of the solar system mentioned at the beginning. However, there are special cases not explained by the theory. 1. Mercury’s large metallic core may be the result of a collision between two planetesimals, where much of ...
... The Role of Catastrophes Condensation-accretion theory explains the 10 properties of the solar system mentioned at the beginning. However, there are special cases not explained by the theory. 1. Mercury’s large metallic core may be the result of a collision between two planetesimals, where much of ...
The Milky Way
... around stars. c. At visible wavelengths, we see disks around the majority of single young stars in the Orion Nebula. d. Both a and b above. e. All of the above. ...
... around stars. c. At visible wavelengths, we see disks around the majority of single young stars in the Orion Nebula. d. Both a and b above. e. All of the above. ...
ph507-16-1exo2
... Direct imaging of planets is difficult because of the enormous difference in brightness between the star and the planet, and the small angular separation between them. Direct detection: must be large and distant from star Circumstellar dust discs. (Circumstantial evidence.) Disc of material around t ...
... Direct imaging of planets is difficult because of the enormous difference in brightness between the star and the planet, and the small angular separation between them. Direct detection: must be large and distant from star Circumstellar dust discs. (Circumstantial evidence.) Disc of material around t ...
Properties of the Planets & Formation of the Solar
... What typical shape(s) do moons have, and why? Although some moons are spherical, most look roughly like potatoes. Those that are spherical are held together by the force of gravity, pulling down high regions. Those that are potato-shaped are held together by the electromagnetic interaction between a ...
... What typical shape(s) do moons have, and why? Although some moons are spherical, most look roughly like potatoes. Those that are spherical are held together by the force of gravity, pulling down high regions. Those that are potato-shaped are held together by the electromagnetic interaction between a ...
View PDF - Sara Seager
... intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will ...
... intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will ...
Planetary system
... been the most successful with a few exoplanets being detected every week this way. Mostly find large Jupiter like planets. The orbits of large planets cause a star to wobble, causing a Doppler effect shifting from red to blue wavelengths. ...
... been the most successful with a few exoplanets being detected every week this way. Mostly find large Jupiter like planets. The orbits of large planets cause a star to wobble, causing a Doppler effect shifting from red to blue wavelengths. ...
Homework 4 1 Chapter 3 October 4, 2011
... helium only condense at colder temperatures. So, close to the sun where it is warmer only the rock and metal could condense and eventually form planets made of those materials. But, farther away the hydrogen and helium condensed as well, so planets in that region are composed of these elements as we ...
... helium only condense at colder temperatures. So, close to the sun where it is warmer only the rock and metal could condense and eventually form planets made of those materials. But, farther away the hydrogen and helium condensed as well, so planets in that region are composed of these elements as we ...
American Scientist
... in the field of astronomy and astrophysics is planet formation: the study of how planets (in our Solar System) and exoplanets (orbiting other stars) form. Astronomers harness the power of telescopes with meter-sized or larger mirrors to search the night sky for exoplanets—and they find loads of them ...
... in the field of astronomy and astrophysics is planet formation: the study of how planets (in our Solar System) and exoplanets (orbiting other stars) form. Astronomers harness the power of telescopes with meter-sized or larger mirrors to search the night sky for exoplanets—and they find loads of them ...
AST 150: Radioactive Dating Game Activity
... Will an extraterrestrial’s signals overlap with the lifespan of the receiving civilization? Extraterrestrials that sent signals a million years ago from a world a million light years away would still overlap ...
... Will an extraterrestrial’s signals overlap with the lifespan of the receiving civilization? Extraterrestrials that sent signals a million years ago from a world a million light years away would still overlap ...
What is a planet?
... The nebular or disk instability hypothesis • the Sun and planets formed together out of a rotating cloud of gas (the solar nebula ) • gravitational instabilities in the gas disk condense into planets (Kant 1755) • Good points: – correctly predicted that stars are surrounded by rotating gas disk ...
... The nebular or disk instability hypothesis • the Sun and planets formed together out of a rotating cloud of gas (the solar nebula ) • gravitational instabilities in the gas disk condense into planets (Kant 1755) • Good points: – correctly predicted that stars are surrounded by rotating gas disk ...
The Association of Dust Disks and Planets Lynne Hillenbrand (Caltech) P.I.
... orbiting farther from their host star, with a 10-year baseline required to detect planets at ∼5 AU. From the known occurrence of giant planets, we expect to discover 10–15 planets from among the 100 “Spitzer” target stars. At least 3 are suspected from the data in hand thusfar. Their masses and orbi ...
... orbiting farther from their host star, with a 10-year baseline required to detect planets at ∼5 AU. From the known occurrence of giant planets, we expect to discover 10–15 planets from among the 100 “Spitzer” target stars. At least 3 are suspected from the data in hand thusfar. Their masses and orbi ...
Mercury_Orbit_Lab_1_(better_than_2)
... How do we know what the orbit of a planet is like? At first glance this appears to be a difficult question, but in many cases it is surprisingly easy to derive an orbit from basic observations. In this exercise you will use a set of simple observations, which you could have made yourself, to discove ...
... How do we know what the orbit of a planet is like? At first glance this appears to be a difficult question, but in many cases it is surprisingly easy to derive an orbit from basic observations. In this exercise you will use a set of simple observations, which you could have made yourself, to discove ...
Article Reference - Archive ouverte UNIGE
... found v sin i = 3.55 ± 0.33 km s−1 . Because this seemed unusually large for this spectral type, we looked at all the stars with a similar B − V present in the HARPS archive: WASP-80 has the widest lines in the sample. There is no significant detection of lithium in the spectrum, and we can place a ...
... found v sin i = 3.55 ± 0.33 km s−1 . Because this seemed unusually large for this spectral type, we looked at all the stars with a similar B − V present in the HARPS archive: WASP-80 has the widest lines in the sample. There is no significant detection of lithium in the spectrum, and we can place a ...
The HARPS search for southern extra-solar planets
... quantitative relation has been established for M dwarfs yet. Bonfils et al. (2007) used variations of these indices to unveil a 35 days rotation period for Gl 674, later confirmed by a photometric campaign, but those of Gl 581 do not measurably vary. The low rotational velocity which we measure for ...
... quantitative relation has been established for M dwarfs yet. Bonfils et al. (2007) used variations of these indices to unveil a 35 days rotation period for Gl 674, later confirmed by a photometric campaign, but those of Gl 581 do not measurably vary. The low rotational velocity which we measure for ...
PHYS178 2008 week 11 part-1
... More sensitive than other techniques to small-mass earth-like planets Most sensitive to planets that have orbits of just several AU’s (such as for Mars or Jupiter/Saturn) The most common stars will be the most likely candidates for lensing Capable of detecting multiple planets in a single light curv ...
... More sensitive than other techniques to small-mass earth-like planets Most sensitive to planets that have orbits of just several AU’s (such as for Mars or Jupiter/Saturn) The most common stars will be the most likely candidates for lensing Capable of detecting multiple planets in a single light curv ...
Lecture 10 - Lick Observatory
... They land at the same time: same acceleration, so same speed when they hit the ground ...
... They land at the same time: same acceleration, so same speed when they hit the ground ...
Kepler (spacecraft)
Kepler is a space observatory launched by NASA to discover Earth-like planets orbiting other stars. The spacecraft, named after the German Renaissance astronomer Johannes Kepler, was launched on March 7, 2009.Designed to survey a portion of our region of the Milky Way to discover dozens of Earth-size extrasolar planets in or near the habitable zone and estimate how many of the billions of stars in the Milky Way have such planets, Kepler's sole instrument is a photometer that continually monitors the brightness of over 145,000 main sequence stars in a fixed field of view. This data is transmitted to Earth, then analyzed to detect periodic dimming caused by extrasolar planets that cross in front of their host star.Kepler is part of NASA's Discovery Program of relatively low-cost, focused primary science missions. The telescope's construction and initial operation were managed by NASA's Jet Propulsion Laboratory, with Ball Aerospace responsible for developing the Kepler flight system. The Ames Research Center is responsible for the ground system development, mission operations since December 2009, and scientific data analysis. The initial planned lifetime was 3.5 years, but greater-than-expected noise in the data, from both the stars and the spacecraft, meant additional time was needed to fulfill all mission goals. Initially, in 2012, the mission was expected to last until 2016, but this would only have been possible if all remaining reaction wheels used for pointing the spacecraft remained reliable. On May 11, 2013, a second of four reaction wheels failed, disabling the collection of science data and threatening the continuation of the mission.On August 15, 2013, NASA announced that they had given up trying to fix the two failed reaction wheels. This meant the current mission needed to be modified, but it did not necessarily mean the end of planet-hunting. NASA had asked the space science community to propose alternative mission plans ""potentially including an exoplanet search, using the remaining two good reaction wheels and thrusters"". On November 18, 2013, the K2 ""Second Light"" proposal was reported. This would include utilizing the disabled Kepler in a way that could detect habitable planets around smaller, dimmer red dwarfs. On May 16, 2014, NASA announced the approval of the K2 extension.As of January 2015, Kepler and its follow-up observations had found 1,013 confirmed exoplanets in about 440 stellar systems, along with a further 3,199 unconfirmed planet candidates. Four planets have been confirmed through Kepler 's K2 mission. In November 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of Sun-like stars and red dwarfs within the Milky Way. It is estimated that 11 billion of these planets may be orbiting Sun-like stars. The nearest such planet may be 3.7 parsecs (12 ly) away, according to the scientists.On January 6, 2015, NASA announced the 1000th confirmed exoplanet discovered by the Kepler Space Telescope. Four of the newly confirmed exoplanets were found to orbit within habitable zones of their related stars: three of the four, Kepler-438b, Kepler-442b and Kepler-452b, are near-Earth-size and likely rocky; the fourth, Kepler-440b, is a super-Earth.