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ASTR 300 Stars and Stellar Systems Spring 2011
... (d) Here we need to consider the triangle formed by the lines from Saturn to to the sun’s center and to it’s edge. This is a “skinny triangle”, so the angle at Saturn (in radians) is given by R⊙/DS , where DS is the distance from the sun to Saturn. Thus angle = R⊙/DS = 7 × 105 km/1.427 × 109 km = 0. ...
... (d) Here we need to consider the triangle formed by the lines from Saturn to to the sun’s center and to it’s edge. This is a “skinny triangle”, so the angle at Saturn (in radians) is given by R⊙/DS , where DS is the distance from the sun to Saturn. Thus angle = R⊙/DS = 7 × 105 km/1.427 × 109 km = 0. ...
NASA has discovered 7 Earth-like planets orbiting a
... our own: small, rocky, and at just the right distance from the star that liquid water could exist on its surface. • That’s why an announcement today from NASA is so exciting: The space agency, along with partners around the world, has found seven potentially Earth-like planets orbiting a star 40 lig ...
... our own: small, rocky, and at just the right distance from the star that liquid water could exist on its surface. • That’s why an announcement today from NASA is so exciting: The space agency, along with partners around the world, has found seven potentially Earth-like planets orbiting a star 40 lig ...
Power point presentation - McMaster Physics and Astronomy
... disks with temperatures (1AU) between 150 and 450 K; and lifetimes between 1 – 10 Million yrs Observe 5-20% of stars with planets in this regime: arises if disk viscosity < 0.0001 ...
... disks with temperatures (1AU) between 150 and 450 K; and lifetimes between 1 – 10 Million yrs Observe 5-20% of stars with planets in this regime: arises if disk viscosity < 0.0001 ...
Contributions of interferometry for Orion
... • Distance is fairly well known (~450pc) • Background contamination is low • Is the paradigm for typical star formation • Is the paradigm for typical planet formation? ...
... • Distance is fairly well known (~450pc) • Background contamination is low • Is the paradigm for typical star formation • Is the paradigm for typical planet formation? ...
The Birth of Stars and Planets
... 1. How does the size distribution and chemical composition of the dust evolve? 2. How does the structure of circumstellar disks evolve (e.g., relative distribution of dust and gas)? 3. Do circumstellar disks show signs of the possible planet formation process or even of the existence of already form ...
... 1. How does the size distribution and chemical composition of the dust evolve? 2. How does the structure of circumstellar disks evolve (e.g., relative distribution of dust and gas)? 3. Do circumstellar disks show signs of the possible planet formation process or even of the existence of already form ...
Solutions3
... Problem 1: The star Mizar in the Big Dipper was the first binary system to be observed (Benedetto Castelli asked Galileo to observe it in 1617, presumably to confirm his observations of this double star)–though not the first where orbital motion was observed. The parallax angle to Mizar is 4.2 × 10− ...
... Problem 1: The star Mizar in the Big Dipper was the first binary system to be observed (Benedetto Castelli asked Galileo to observe it in 1617, presumably to confirm his observations of this double star)–though not the first where orbital motion was observed. The parallax angle to Mizar is 4.2 × 10− ...
Document
... (spheromaks) that become planetary cores. The reconnection radiation and winds heat and compress the disk causing agglomeration out to the snow line. The cores grow by collecting material infalling toward the star. They are in unstable orbits that can change radically or they can be ejected from the ...
... (spheromaks) that become planetary cores. The reconnection radiation and winds heat and compress the disk causing agglomeration out to the snow line. The cores grow by collecting material infalling toward the star. They are in unstable orbits that can change radically or they can be ejected from the ...
TheExoplanet and the Amateurs
... Based on the gravitational tug detected in its host star, HD 17156b has a mass of 3.1 Jupiters. The amount of starlight it blocks indicates that its diameter is about 1.15 Jupiters. Theorists can breathe a sigh of relief, because the calculated average density, roughly 2.6 times the density of water ...
... Based on the gravitational tug detected in its host star, HD 17156b has a mass of 3.1 Jupiters. The amount of starlight it blocks indicates that its diameter is about 1.15 Jupiters. Theorists can breathe a sigh of relief, because the calculated average density, roughly 2.6 times the density of water ...
Planetary Overview Inventory How the Planets fit Bode`s Law
... temperatures of over 1000ºC facing the star Detecting Earth-like planets will not be easy 47 UMa has at least 2 giant planets in circular orbit at a distance of several AU a new era in astronomy has dawned new instruments, including giant mirrors and custom designed ...
... temperatures of over 1000ºC facing the star Detecting Earth-like planets will not be easy 47 UMa has at least 2 giant planets in circular orbit at a distance of several AU a new era in astronomy has dawned new instruments, including giant mirrors and custom designed ...
Debris Disk Imaging - Institute of Astronomy
... For example, extended structure of AU Mic (Krist 2005) explained by dust created in a narrow belt at ~40AU ...
... For example, extended structure of AU Mic (Krist 2005) explained by dust created in a narrow belt at ~40AU ...
Formation of planetary systems Protoplanetary disks contain dust
... Rocky planetesimals Rocky and icy planetesimals Snow line at r ~ 3 au • Surface density of planetesimals is larger beyond the snow line, in parts of the disk cool enough for ice to be present • Higher surface density -> more rapid formation of planets • In the outer Solar System, planets grew to ~20 ...
... Rocky planetesimals Rocky and icy planetesimals Snow line at r ~ 3 au • Surface density of planetesimals is larger beyond the snow line, in parts of the disk cool enough for ice to be present • Higher surface density -> more rapid formation of planets • In the outer Solar System, planets grew to ~20 ...
Kepler Orbits Kepler Orbits
... • Measure star’s motion in the plane of the sky due to the orbiting planet • Must correct measurements for parallax and proper motion of star • Doppler (radial velocity) more sensitive to planets close to the star • Astrometry more sensitive to planets far from the star ...
... • Measure star’s motion in the plane of the sky due to the orbiting planet • Must correct measurements for parallax and proper motion of star • Doppler (radial velocity) more sensitive to planets close to the star • Astrometry more sensitive to planets far from the star ...
Astronomy 321 --- Homework Exercise: Star Wheel
... stars? State both the cardinal direction (e.g., SW or ENE) and the altitude, i.e., how high above the horizon the object is in degrees, approximately. Remember that the altitude is 0° at the horizon and 90° at the zenith. the constellation Sagittarius: the constellation Cygnus: the star Antares in S ...
... stars? State both the cardinal direction (e.g., SW or ENE) and the altitude, i.e., how high above the horizon the object is in degrees, approximately. Remember that the altitude is 0° at the horizon and 90° at the zenith. the constellation Sagittarius: the constellation Cygnus: the star Antares in S ...
July 14, 2003
... planets outside of the solar system — but all of those are about the same age or just slightly older than the sun, 4.5 billion years. It was thought that planets could not form until there had been at least one generation of stars after the big bang because the planet building requires heavier eleme ...
... planets outside of the solar system — but all of those are about the same age or just slightly older than the sun, 4.5 billion years. It was thought that planets could not form until there had been at least one generation of stars after the big bang because the planet building requires heavier eleme ...
Interstellar Medium (ISM) Star Formation Formation of Planetary Systems
... Clearing the Protosolar Nebula Four effects cleared the nebula: 1. Radiation pressure-light streaming from the sun pushed against the particles of the solar nebula. 2. The solar wind—flow of ionized H helped push dust and gas out of the nebula. 3. Sweeping of space debris by the planets—the moon ...
... Clearing the Protosolar Nebula Four effects cleared the nebula: 1. Radiation pressure-light streaming from the sun pushed against the particles of the solar nebula. 2. The solar wind—flow of ionized H helped push dust and gas out of the nebula. 3. Sweeping of space debris by the planets—the moon ...
Document
... • How common are planets around stars? • How common are rocky planets? • How common are planets in the habitable zone? o where liquid water can exist • How common is water? • How common are biomarkers? ...
... • How common are planets around stars? • How common are rocky planets? • How common are planets in the habitable zone? o where liquid water can exist • How common is water? • How common are biomarkers? ...
Astronomers discover a highly inflated sub
... observations from the Spitzer Space Telescope to better measure the planet properties, and they are currently discussing observations with the Hubble Space Telescope and other observatories to star probing the planet's atmosphere. More information: KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Tr ...
... observations from the Spitzer Space Telescope to better measure the planet properties, and they are currently discussing observations with the Hubble Space Telescope and other observatories to star probing the planet's atmosphere. More information: KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Tr ...
Deep Sky Objects (Word)
... planet is only 0.8 days. What is the semi-major axis of its orbit in AU? 16. The host star of WASP-18b is an F6 star with a mass of 1.25 solar masses. The planet orbits with a semi-major axis of only 0.020 AU and a period of 0.94 days. What is the estimated mass of the planet and how does it compare ...
... planet is only 0.8 days. What is the semi-major axis of its orbit in AU? 16. The host star of WASP-18b is an F6 star with a mass of 1.25 solar masses. The planet orbits with a semi-major axis of only 0.020 AU and a period of 0.94 days. What is the estimated mass of the planet and how does it compare ...
The Rocket Science of Launching Stellar Disks
... – Driven by line-scattering of star’s radiation – Rotation can lead to Wind Compressed Disk (WCD) – But still lacks angular momentum for orbit ...
... – Driven by line-scattering of star’s radiation – Rotation can lead to Wind Compressed Disk (WCD) – But still lacks angular momentum for orbit ...
23.4 Physical processes, heating and cooling … (HB)
... Distribution of Mass and Angular Momentum: Sun Mass: 99.86% but Angular Momentum <2% Age estimation: Sun and Planets have been formed at the same time ...
... Distribution of Mass and Angular Momentum: Sun Mass: 99.86% but Angular Momentum <2% Age estimation: Sun and Planets have been formed at the same time ...
Lec11_2D
... Accretion Disks and Black Holes The accretion disk around a black hole can extend very close to the event horizon. The gas speed there is very close to the speed of light, so the friction in the disk is extremely intense. This type of disk will produce the most-energetic x-rays. ...
... Accretion Disks and Black Holes The accretion disk around a black hole can extend very close to the event horizon. The gas speed there is very close to the speed of light, so the friction in the disk is extremely intense. This type of disk will produce the most-energetic x-rays. ...
doc - EU-HOU
... method; hence it helps its classification. Light curve of an exoplanet transit observed by the Corot telescope (May 2007) ...
... method; hence it helps its classification. Light curve of an exoplanet transit observed by the Corot telescope (May 2007) ...
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. ...
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.