two new very hot jupiters in the flames spotlight
... Since the pioneering discovery of 51Peg B by Mayor and Queloz in 1995, more than 120 extra-solar planets have been discovered so far. Almost all of them have in common the fact that their presence was revealed by radial velocity surveys, which consist in the monitoring of the periodic wobble of the ...
... Since the pioneering discovery of 51Peg B by Mayor and Queloz in 1995, more than 120 extra-solar planets have been discovered so far. Almost all of them have in common the fact that their presence was revealed by radial velocity surveys, which consist in the monitoring of the periodic wobble of the ...
Astronomical Art
... ‘exoplanets’ (a planet which orbits a star outside the solar system) could look like. Helena has used the online tool Endeavour (http://www.astronexus.com/ endeavour) to meticulously plot where stars would appear in the skies of these distant planets. Using this online tool to inspire her paintings ...
... ‘exoplanets’ (a planet which orbits a star outside the solar system) could look like. Helena has used the online tool Endeavour (http://www.astronexus.com/ endeavour) to meticulously plot where stars would appear in the skies of these distant planets. Using this online tool to inspire her paintings ...
NASA`s Kepler Discovers Its Smallest `Habitable Zone` Planets to
... new planetary systems that include three super-Earth-size planets in the "habitable zone," the range of distance from a star where the surface temperature of an orbiting planet might be suitable for liquid water. The Kepler-62 system has five planets; 62b, 62c, 62d, 62e and 62f. The Kepler-69 system ...
... new planetary systems that include three super-Earth-size planets in the "habitable zone," the range of distance from a star where the surface temperature of an orbiting planet might be suitable for liquid water. The Kepler-62 system has five planets; 62b, 62c, 62d, 62e and 62f. The Kepler-69 system ...
Kepler Team Finds System with Two Potentially Habitable Planets
... “These planets are unlike anything in our solar system. They have endless oceans,” said lead author Lisa Kaltenegger of the Max Planck Institute for Astronomy and the Harvard Smithsonian Center for Astrophysics. “There may be life there, but could it be technology-based like ours? Life on these worl ...
... “These planets are unlike anything in our solar system. They have endless oceans,” said lead author Lisa Kaltenegger of the Max Planck Institute for Astronomy and the Harvard Smithsonian Center for Astrophysics. “There may be life there, but could it be technology-based like ours? Life on these worl ...
Extrasolar Planets
... Extrasolar Planet = Exoplanet = Planet orbiting a star other than the Sun. ...
... Extrasolar Planet = Exoplanet = Planet orbiting a star other than the Sun. ...
ASTR 300 Stars and Stellar Systems Spring 2011
... angular momentum and energy away. Thus a very rapidly spinning pulsar was assumed to be very young. Later they realized that an old, slowly spinning pulsar could be “spun up” by mass transfer from a companion star. 4. What is “The Black Widow” pulsar and what puzzling objects does it help explain? “ ...
... angular momentum and energy away. Thus a very rapidly spinning pulsar was assumed to be very young. Later they realized that an old, slowly spinning pulsar could be “spun up” by mass transfer from a companion star. 4. What is “The Black Widow” pulsar and what puzzling objects does it help explain? “ ...
Extreme Stars
... Only certain combinations of size and mass are stable Stars will shrink or expand to reach stability ...
... Only certain combinations of size and mass are stable Stars will shrink or expand to reach stability ...
Orbits Sample Calculation Word Document | GCE AS/A
... Orbital speed of star: vS = 1830.7 ± 2.2 m s1 Orbital period T = 168.848 ± 0.030 days [N.B. Ignore the uncertainty figures; they are only included to give an idea of the accuracies involved] Use the same method to show that the mass of the companion is about 25 Jupiter masses and therefore is likel ...
... Orbital speed of star: vS = 1830.7 ± 2.2 m s1 Orbital period T = 168.848 ± 0.030 days [N.B. Ignore the uncertainty figures; they are only included to give an idea of the accuracies involved] Use the same method to show that the mass of the companion is about 25 Jupiter masses and therefore is likel ...
NASA has discovered 7 Earth-like planets orbiting a
... they update their estimates of how many Earth-like planets could be out there. “For every transiting planet found, there should be a multitude of similar planets (20–100 times more) that, seen from Earth, never pass in front of their host star,” Nature reporter Ignas Snellen explains in a feature ar ...
... they update their estimates of how many Earth-like planets could be out there. “For every transiting planet found, there should be a multitude of similar planets (20–100 times more) that, seen from Earth, never pass in front of their host star,” Nature reporter Ignas Snellen explains in a feature ar ...
Kepler Orbits Kepler Orbits
... • Achieved by passing stellar light through a cell containing iodine, imprinting large number of additional lines of known wavelength into the spectrum. • Calibration suffers identical instrumental distortions as the data ...
... • Achieved by passing stellar light through a cell containing iodine, imprinting large number of additional lines of known wavelength into the spectrum. • Calibration suffers identical instrumental distortions as the data ...
Extrasolar Planets - University of New South Wales
... - The effect is greatest for large mass planet in very close in orbits - Requires us to observe for at least one full orbit (Jupiter = 12 years) - Requires high precision, placing lower limits on the size of the signal we can detect ...
... - The effect is greatest for large mass planet in very close in orbits - Requires us to observe for at least one full orbit (Jupiter = 12 years) - Requires high precision, placing lower limits on the size of the signal we can detect ...
poster
... above the circum-stellar absorption layer. We constrain the model space from the observed X-ray parameters and, adding information from the literature, we build a physical model that interprets the X-ray emission in terms of an outflow. We find that only a very small fraction of the total mass loss ...
... above the circum-stellar absorption layer. We constrain the model space from the observed X-ray parameters and, adding information from the literature, we build a physical model that interprets the X-ray emission in terms of an outflow. We find that only a very small fraction of the total mass loss ...
Review Game
... 11) Refering to Diagram 1, compared to the original planet (Graph 1) which graph shows a planet orbiting faster? 12) Refering to Diagram 1, compared to the original planet graph (Graph 1) which graph shows a larger planet? 13) About how long ago were the first planets around other Sun-like stars we ...
... 11) Refering to Diagram 1, compared to the original planet (Graph 1) which graph shows a planet orbiting faster? 12) Refering to Diagram 1, compared to the original planet graph (Graph 1) which graph shows a larger planet? 13) About how long ago were the first planets around other Sun-like stars we ...
Laboratory Procedure (Word Format)
... the shift will be to shorter wavelengths (blue shift) by the same amount. In our ideal case, the measured Doppler velocity would be equal to the earth’s orbital velocity. In an actual application of the method, there are some complications: 1. The star may not be stationary with respect to the sun, ...
... the shift will be to shorter wavelengths (blue shift) by the same amount. In our ideal case, the measured Doppler velocity would be equal to the earth’s orbital velocity. In an actual application of the method, there are some complications: 1. The star may not be stationary with respect to the sun, ...
The Sun and Planets Homework 9.
... does this technique work best for detecting massive planets, and those in short period orbits around their host star? What planetary parameters can you determine using this technique? 2. Briefly explain the transit method for detecting extrasolar planets. What type of planets is this technique most ...
... does this technique work best for detecting massive planets, and those in short period orbits around their host star? What planetary parameters can you determine using this technique? 2. Briefly explain the transit method for detecting extrasolar planets. What type of planets is this technique most ...
ISO Adds a Critical Ingredient to the Jovian Planet
... years, and have led to the view that gas-giant planet formation must take place very rapidly, on time scales that are difficult to understand theoretically. This is where Blake and collaborators enter the picture. Using the Short Wavelength Spectrometer on ISO, they have found large amounts of gas i ...
... years, and have led to the view that gas-giant planet formation must take place very rapidly, on time scales that are difficult to understand theoretically. This is where Blake and collaborators enter the picture. Using the Short Wavelength Spectrometer on ISO, they have found large amounts of gas i ...
Other Worlds - UC Berkeley Astronomy w
... naked eye. Distance ~ 50 ly • Technology at optical wavelengths is not yet good enough (usually) to detect Earth-sized planets • We preferentially find very small orbits, high eccentricities, and massive planets because these produce the greatest Doppler shift. • Most of these planets are unlike any ...
... naked eye. Distance ~ 50 ly • Technology at optical wavelengths is not yet good enough (usually) to detect Earth-sized planets • We preferentially find very small orbits, high eccentricities, and massive planets because these produce the greatest Doppler shift. • Most of these planets are unlike any ...
Discovery of Extrasolar Planets - WSU Astronomy.
... around which the planets orbit are not too different from the sun. They are nearby, often fairly bright, and some of them have been in star catalogs for centuries. We detect planets around them by the reflex motion of the star caused by the gravitational tug of the planet. In the illustration above, ...
... around which the planets orbit are not too different from the sun. They are nearby, often fairly bright, and some of them have been in star catalogs for centuries. We detect planets around them by the reflex motion of the star caused by the gravitational tug of the planet. In the illustration above, ...
Habitability: Good, Bad and the Ugly
... – Several stars in our galaxy with planets the size of Jupiter within terrestrial zone from their sun – Mass of star • Larger mass, greater luminosity, shorter life • Most abundant stars in galaxy are least luminous and longest-lived (red dwarfs) ...
... – Several stars in our galaxy with planets the size of Jupiter within terrestrial zone from their sun – Mass of star • Larger mass, greater luminosity, shorter life • Most abundant stars in galaxy are least luminous and longest-lived (red dwarfs) ...
Enceladus is small (500 km diameter)
... Around Epsilon Indi (Spectral type K5: about one-tenth the Sun's luminosity), an Earth-sized planet would have to orbit at about the distance of Mercury from the star. ...
... Around Epsilon Indi (Spectral type K5: about one-tenth the Sun's luminosity), an Earth-sized planet would have to orbit at about the distance of Mercury from the star. ...
March 2016
... Exoplanets are planets orbiting stars other than our sun. Some of their orbits lie in our line of sight, so they transit across the face of their star from our point of view. Observations of the amount of light blocked, and the duration of the transit allow us to calculate the radius of the planet a ...
... Exoplanets are planets orbiting stars other than our sun. Some of their orbits lie in our line of sight, so they transit across the face of their star from our point of view. Observations of the amount of light blocked, and the duration of the transit allow us to calculate the radius of the planet a ...
Lecture22 - Indiana University Astronomy
... Around Epsilon Indi (Spectral type K5: about one-tenth the Sun's luminosity), an Earth-sized planet would have to orbit at about the distance of Mercury from the star. ...
... Around Epsilon Indi (Spectral type K5: about one-tenth the Sun's luminosity), an Earth-sized planet would have to orbit at about the distance of Mercury from the star. ...
Diapositiva 1
... orbit inclination along the line of sight, and on the mass ratio between the two objects (assuming the simple case of only two bodies). This approach takes benefits from the Doppler effect. For example, Jupiter ‘produces’ on the Sun an effect of about 12 m/s. ...
... orbit inclination along the line of sight, and on the mass ratio between the two objects (assuming the simple case of only two bodies). This approach takes benefits from the Doppler effect. For example, Jupiter ‘produces’ on the Sun an effect of about 12 m/s. ...
Tau Ceti
Tau Ceti (τ Cet, τ Ceti) is a star in the constellation Cetus that is spectrally similar to the Sun, although it has only about 78% of the Sun's mass. At a distance of just under 12 light-years from the Solar System, it is a relatively nearby star, and is the closest solitary G-class star. The star appears stable, with little stellar variation, and is metal-deficient.Observations have detected more than ten times as much dust surrounding Tau Ceti as is present in the Solar System. Since December 2012, there has been evidence of possibly five planets orbiting Tau Ceti, with two of these being potentially in the habitable zone. Because of its debris disk, any planet orbiting Tau Ceti would face far more impact events than Earth. Despite this hurdle to habitability, its solar analog (Sun-like) characteristics have led to widespread interest in the star. Given its stability, similarity and relative proximity to the Sun, Tau Ceti is consistently listed as a target for the Search for Extra-Terrestrial Intelligence (SETI), and it appears in some science fiction literature.It can be seen with the unaided eye as a third-magnitude star. As seen from Tau Ceti, the Sun would be a third-magnitude star in the constellation Boötes.