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 ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... KEPLER is 1-dimensional (meaning it assumes that stars are spherical, so physical quantities such as temperature or density can depend only on radius). KEPLER follows how gas turns into stars and how supernovae feed back energy into surrounding gas; it also traces how convection—movement of gas insi ...
... KEPLER is 1-dimensional (meaning it assumes that stars are spherical, so physical quantities such as temperature or density can depend only on radius). KEPLER follows how gas turns into stars and how supernovae feed back energy into surrounding gas; it also traces how convection—movement of gas insi ...
Phobos
... imply that the Hubble constant should be correspondingly reduced and that the Universe could be 15% bigger and older. The astronomers studied two of the brightest stars in M33, the components of a binary system in which one star eclipses the other every five days. They determined the masses of the c ...
... imply that the Hubble constant should be correspondingly reduced and that the Universe could be 15% bigger and older. The astronomers studied two of the brightest stars in M33, the components of a binary system in which one star eclipses the other every five days. They determined the masses of the c ...
Stellar Evolution (Formation)
... When the core’s H is exhausted, there will be no more nuclear energy to heat the gas. Gravity will win over gas pressure and the core will collapse. Gravitational potential energy of the core will be converted to heat as it shrinks. This new heat source will trigger new fusion reactions: (3-) ...
... When the core’s H is exhausted, there will be no more nuclear energy to heat the gas. Gravity will win over gas pressure and the core will collapse. Gravitational potential energy of the core will be converted to heat as it shrinks. This new heat source will trigger new fusion reactions: (3-) ...
Measuring Our Universe
... any planet to the Sun in terms of Earth’s distance, the AU, from that planet’s orbital period, its year. By obtaining an accurate value of AU, Cassini unlocked the distances and sizes of other planets in the solar system. This gave us, for the first time in the history of our species, an accurate un ...
... any planet to the Sun in terms of Earth’s distance, the AU, from that planet’s orbital period, its year. By obtaining an accurate value of AU, Cassini unlocked the distances and sizes of other planets in the solar system. This gave us, for the first time in the history of our species, an accurate un ...
Solutions - faculty.ucmerced.edu
... 1. (a) Assuming that the surface temperature of the Sun is T = 5800 K, use Stefan’s law to determine the rest mass lost per second to radiation by the Sun. Take the Sun’s radius to be R = 7.0 × 108 meters. (b) What fraction of the Sun’s rest mass is lost each year from electromagnetic radiation? T ...
... 1. (a) Assuming that the surface temperature of the Sun is T = 5800 K, use Stefan’s law to determine the rest mass lost per second to radiation by the Sun. Take the Sun’s radius to be R = 7.0 × 108 meters. (b) What fraction of the Sun’s rest mass is lost each year from electromagnetic radiation? T ...
Physics: Forces and Motion
... 3. Use models to explain how Earth’s revolution around the sun affects changes in daylight hours and seasonal temperatures. 4. Compare the revolution times of planets and relate them to distance from the sun. 5. Design and conduct a scientific simulation to explore the relationship between the angle ...
... 3. Use models to explain how Earth’s revolution around the sun affects changes in daylight hours and seasonal temperatures. 4. Compare the revolution times of planets and relate them to distance from the sun. 5. Design and conduct a scientific simulation to explore the relationship between the angle ...
Black Hole vs. Earth
... •! For the rest of the Solar System, it will depend on the orbits. •! If the black hole doesn’t get close to the Sun, it will be fine, otherwise, it may get torn apart too. •! Then, the black hole likely moves on. ...
... •! For the rest of the Solar System, it will depend on the orbits. •! If the black hole doesn’t get close to the Sun, it will be fine, otherwise, it may get torn apart too. •! Then, the black hole likely moves on. ...
Theoretical Problem 3
... The stars are spheres of hot gas. Most of them shine because they are fusing hydrogen into helium in their central parts. In this problem we use concepts of both classical and quantum mechanics, as well as of electrostatics and thermodynamics, to understand why stars have to be big enough to achieve ...
... The stars are spheres of hot gas. Most of them shine because they are fusing hydrogen into helium in their central parts. In this problem we use concepts of both classical and quantum mechanics, as well as of electrostatics and thermodynamics, to understand why stars have to be big enough to achieve ...
Jupiter and Saturn Guiding Questions Long orbital periods of Jupiter
... • This system is tilted away from the plane of Saturn’s orbit, which causes the rings to be seen at various angles by an Earth-based observer over the course of a Saturnian year ...
... • This system is tilted away from the plane of Saturn’s orbit, which causes the rings to be seen at various angles by an Earth-based observer over the course of a Saturnian year ...
Lecture13.v2 - Lick Observatory
... gravity strongly perturbed the orbits of almost all the asteroids • Most of them got nudged into highly eccentric orbits, from which they either leave the Solar System or head inwards toward the Sun • A fraction of the asteroids headed inwards may have hit the early Earth! Page 23 ...
... gravity strongly perturbed the orbits of almost all the asteroids • Most of them got nudged into highly eccentric orbits, from which they either leave the Solar System or head inwards toward the Sun • A fraction of the asteroids headed inwards may have hit the early Earth! Page 23 ...
Sample pages 2 PDF
... that the total estimated mass of all the asteroids combined would present an object of around 1497 km in diameter that, in itself, would cause a problem of classification, as the body would be less than half the size of our own Moon. However, the formation would have taken place long before anyone ev ...
... that the total estimated mass of all the asteroids combined would present an object of around 1497 km in diameter that, in itself, would cause a problem of classification, as the body would be less than half the size of our own Moon. However, the formation would have taken place long before anyone ev ...
Exploring the Moon and Stars
... Exploration 10: Modeling Moon Phases • The phase or appearance of the Moon depends upon the relative positions of the Earth, Moon, and Sun. • The Moon is illuminated by sunlight. • The portions of the Moon facing the Earth but not visible during many of the phases are hidden in the Moon’s own shadow ...
... Exploration 10: Modeling Moon Phases • The phase or appearance of the Moon depends upon the relative positions of the Earth, Moon, and Sun. • The Moon is illuminated by sunlight. • The portions of the Moon facing the Earth but not visible during many of the phases are hidden in the Moon’s own shadow ...
Name - crespiphysics
... actually absorb? As a result, what is the earth’s average temperature in degrees Fahrenheit (yes, I’m making you perform a conversion!)? What would the earth’s average temperature be (again in degrees Fahrenheit) if it absorbed 100% of the energy falling on it? ...
... actually absorb? As a result, what is the earth’s average temperature in degrees Fahrenheit (yes, I’m making you perform a conversion!)? What would the earth’s average temperature be (again in degrees Fahrenheit) if it absorbed 100% of the energy falling on it? ...
Stargazer - Everett Astronomical Society
... most enigmatic landforms in the solar system. The deep canyons spiraling out from Red Planet's North and South poles cover hundreds of miles. No other planet has such structures. A new model of trough formation suggests that heating and cooling alone are sufficient to form the unusual patterns. Prev ...
... most enigmatic landforms in the solar system. The deep canyons spiraling out from Red Planet's North and South poles cover hundreds of miles. No other planet has such structures. A new model of trough formation suggests that heating and cooling alone are sufficient to form the unusual patterns. Prev ...
May - Fort Worth Astronomical Society
... Mercury: Look for this elusive planet during the first 10 days of May, shining at almost 0 magnitude low in the western sky at sunset. It reaches its greatest height above the horizon on the evening of May 3. Venus: Other than the moon, Venus is the brightest object in the sky. You can't miss it! Lo ...
... Mercury: Look for this elusive planet during the first 10 days of May, shining at almost 0 magnitude low in the western sky at sunset. It reaches its greatest height above the horizon on the evening of May 3. Venus: Other than the moon, Venus is the brightest object in the sky. You can't miss it! Lo ...
Sample pages 2 PDF
... still be seen in the Crab nebula, of which a picture appears in Fig. 2.4. The supernovae are significant because they produce the elements above iron in the periodic table and because they spread the products of nuclear burning in the interior of stars into the interstellar medium. Assuming that, li ...
... still be seen in the Crab nebula, of which a picture appears in Fig. 2.4. The supernovae are significant because they produce the elements above iron in the periodic table and because they spread the products of nuclear burning in the interior of stars into the interstellar medium. Assuming that, li ...
Powerpoint
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
Star in a Box - Las Cumbres Observatory Global Telescope
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
... •Luminosity up the vertical axis (measured relative to the Sun) •Temperature along the horizontal axis (measured in Kelvin) The stars Vega and Sirius are brighter than the Sun, and also hotter. Where would you put them? Where would you mark the Sun on the plot? ...
Neutron Star - Perry Local Schools
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
Historical Overview of the Universe
... catalogued, and the spectroscopic decomposition of light was learned as the first astrophysical method. In the twentieth century, stellar spectroscopy was developed as a way of determining stellar parameters, in particular the abundances of the chemical elements. Computer simulations of the evolutio ...
... catalogued, and the spectroscopic decomposition of light was learned as the first astrophysical method. In the twentieth century, stellar spectroscopy was developed as a way of determining stellar parameters, in particular the abundances of the chemical elements. Computer simulations of the evolutio ...
PLANETESIMALS TO BROWN DWARFS: What is a Planet?
... (exoplanets). The first exoplanets discovered are actually terrestrial, but were found in orbit around a neutron star (Wolszczan & Frail 1992). These clearly have a very different history from planets in our Solar System because their current orbits would have been inside the supergiant star that pre ...
... (exoplanets). The first exoplanets discovered are actually terrestrial, but were found in orbit around a neutron star (Wolszczan & Frail 1992). These clearly have a very different history from planets in our Solar System because their current orbits would have been inside the supergiant star that pre ...
Formation and evolution of the Solar System
The formation of the Solar System began 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the Sun, while the rest flattened into a protoplanetary disk out of which the planets, moons, asteroids, and other small Solar System bodies formed.This widely accepted model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, physics, geology, and planetary science. Since the dawn of the space age in the 1950s and the discovery of extrasolar planets in the 1990s, the model has been both challenged and refined to account for new observations.The Solar System has evolved considerably since its initial formation. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are thought to have formed independently and later been captured by their planets. Still others, such as the Moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been central to the evolution of the Solar System. The positions of the planets often shifted due to gravitational interactions. This planetary migration is now thought to have been responsible for much of the Solar System's early evolution.In roughly 5 billion years, the Sun will cool and expand outward many times its current diameter (becoming a red giant), before casting off its outer layers as a planetary nebula and leaving behind a stellar remnant known as a white dwarf. In the far distant future, the gravity of passing stars will gradually reduce the Sun's retinue of planets. Some planets will be destroyed, others ejected into interstellar space. Ultimately, over the course of tens of billions of years, it is likely that the Sun will be left with none of the original bodies in orbit around it.