Hydrogen Greenhouse Planets Beyond the Habitable Zone
... planets around M stars will be below the condensation temperature of all gases except for H2 and He. These mono- and di-atomic gases lack the bending and rotational modes that impart features to the infrared absorption spectra of more complex molecules. At high pressure, however, collisions cause H2 ...
... planets around M stars will be below the condensation temperature of all gases except for H2 and He. These mono- and di-atomic gases lack the bending and rotational modes that impart features to the infrared absorption spectra of more complex molecules. At high pressure, however, collisions cause H2 ...
No Slide Title
... a long time.It was a Supernova and we see the remnants in these pictures.The first four show it as seen in four different regions of the electromagnetic spectrum[UV,visible,IR,X-ray].The final picture shows detail.The bright clumps of light are moving outwards at v = 0.5c.The filaments have lower ma ...
... a long time.It was a Supernova and we see the remnants in these pictures.The first four show it as seen in four different regions of the electromagnetic spectrum[UV,visible,IR,X-ray].The final picture shows detail.The bright clumps of light are moving outwards at v = 0.5c.The filaments have lower ma ...
Standard EPS Shell Presentation
... The universe continued as a giant cloud of gas until about 300 million years after the Big Bang. Parts of the gas cloud began to collapse and ignite to form clusters of stars—the first galaxies. ...
... The universe continued as a giant cloud of gas until about 300 million years after the Big Bang. Parts of the gas cloud began to collapse and ignite to form clusters of stars—the first galaxies. ...
BENNETT, Constraints on the Orbital Motion of OGLE-2006
... distance, and velocity) are constrained by the Einstein radius crossing time, tE • There are two ways to improve upon this with light curve data: – Determine the angular Einstein radius : E= *tE/t* = tErel where * is the angular radius of the star and rel is the relative lens-source proper moti ...
... distance, and velocity) are constrained by the Einstein radius crossing time, tE • There are two ways to improve upon this with light curve data: – Determine the angular Einstein radius : E= *tE/t* = tErel where * is the angular radius of the star and rel is the relative lens-source proper moti ...
Exam Name___________________________________
... 65) A cloud fragment too small to collapse into a main sequence star becomes a A) planet of another star. B) brown dwarf. C) pulsar. D) white dwarf. E) T-Tauri object. ...
... 65) A cloud fragment too small to collapse into a main sequence star becomes a A) planet of another star. B) brown dwarf. C) pulsar. D) white dwarf. E) T-Tauri object. ...
N (North) Equator Latitude and Declination
... The observed altitude of a star is its angular distance above the observer’s horizon. A star’s altitude will vary with the time of observation. A star’s declination is its angular distance above the celestial equator. The declination is also 90 degrees minus the angle the star makes with the earth’s ...
... The observed altitude of a star is its angular distance above the observer’s horizon. A star’s altitude will vary with the time of observation. A star’s declination is its angular distance above the celestial equator. The declination is also 90 degrees minus the angle the star makes with the earth’s ...
here - Atomki
... - Astrometry → distance - Eclipsing binaries → mass ratios, orbital info - Occultations & interferometry → angular diameter, R - Seismology → interior structure: c s, ρ, ... ...
... - Astrometry → distance - Eclipsing binaries → mass ratios, orbital info - Occultations & interferometry → angular diameter, R - Seismology → interior structure: c s, ρ, ... ...
The Mass Assembly of Galaxies
... There is a cluster of B stars in the central 1’’ of the galaxy, the so-called S-cluster. These high proper motion stars - in particular star S2 - show that Sgr A* is a black-hole of 3-4 million solar masses. Large numbers of young stars, in particular O supergiants and WR stars are observed within 2 ...
... There is a cluster of B stars in the central 1’’ of the galaxy, the so-called S-cluster. These high proper motion stars - in particular star S2 - show that Sgr A* is a black-hole of 3-4 million solar masses. Large numbers of young stars, in particular O supergiants and WR stars are observed within 2 ...
Astrophysics E1. This question is about stars.
... (iii) Light from Vega is absorbed by a dust cloud between Vega and Earth. Suggest the effect, if any, this will have on determining the distance of Vega from Earth. ...
... (iii) Light from Vega is absorbed by a dust cloud between Vega and Earth. Suggest the effect, if any, this will have on determining the distance of Vega from Earth. ...
Topics for this week
... The best way to explain how nuclear reactions generate energy is to note that a helium atom has less mass than the 4 hydrogen atoms that were fused to make it. Einstein’s famous equation, E = m c2, says that mass can be converted into energy (or energy into mass) and to calculate the energy generate ...
... The best way to explain how nuclear reactions generate energy is to note that a helium atom has less mass than the 4 hydrogen atoms that were fused to make it. Einstein’s famous equation, E = m c2, says that mass can be converted into energy (or energy into mass) and to calculate the energy generate ...
Powerpoint
... Planetary formation has begun, but the protostar is still not in equilibrium – all heating comes from the gravitational collapse. ...
... Planetary formation has begun, but the protostar is still not in equilibrium – all heating comes from the gravitational collapse. ...
AST301.Ch16.Sun
... 1. Theoretical modeling—e.g. hydrostatic equilibrium (pressure balances gravity), energy conservation through each layer… This gives the values of temperature, pressure, density, luminosity as a function of radius, from the center to the photosphere. This is the only way to get detailed predictions ...
... 1. Theoretical modeling—e.g. hydrostatic equilibrium (pressure balances gravity), energy conservation through each layer… This gives the values of temperature, pressure, density, luminosity as a function of radius, from the center to the photosphere. This is the only way to get detailed predictions ...
File
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
File - Awakening in Grade 6
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
Planetary Nebula NGC 7027 Hubble Space Telescope
... infrared image (on the left) shows a young planetary nebula in a state o f rapid transition. This image alone reveals important new information. When astronomers combine this photo with an earlier image taken in visible light, they have a more complete picture of the final stages of star life. NGC 7 ...
... infrared image (on the left) shows a young planetary nebula in a state o f rapid transition. This image alone reveals important new information. When astronomers combine this photo with an earlier image taken in visible light, they have a more complete picture of the final stages of star life. NGC 7 ...
Extraterrestrial Life
... Fs – fraction of stars with properties for life to develop • Water is probably essential as a solvent. So, planet must have exact temperature (distance from the star) to have water (liquid state). Between 273 K and 373 K. • Pressure must be right too (atmosphere weights the equivalent to 3 elephants ...
... Fs – fraction of stars with properties for life to develop • Water is probably essential as a solvent. So, planet must have exact temperature (distance from the star) to have water (liquid state). Between 273 K and 373 K. • Pressure must be right too (atmosphere weights the equivalent to 3 elephants ...
Measuring stars Part I
... Deneb has an Absolute visual magnitude of -8.73 (this is about the same brightness as the quarter moon---but at 32.6 light years away!) Using the weird equation, the distance to deneb can be calculated: 2500 light years (M – m = 5 – 5log(d)) One last obvious question: How did we ever know the Absolu ...
... Deneb has an Absolute visual magnitude of -8.73 (this is about the same brightness as the quarter moon---but at 32.6 light years away!) Using the weird equation, the distance to deneb can be calculated: 2500 light years (M – m = 5 – 5log(d)) One last obvious question: How did we ever know the Absolu ...
Stefan-Boltzmann Law
... temperature? (This is meant to be obvious.) Which lettered example(s) above supports your answer? 4. If you use two hot plates of different sizes, can you assume that the one that boils water first is at a higher temperature? Which lettered example(s) above supports your answer? 5. Two students are ...
... temperature? (This is meant to be obvious.) Which lettered example(s) above supports your answer? 4. If you use two hot plates of different sizes, can you assume that the one that boils water first is at a higher temperature? Which lettered example(s) above supports your answer? 5. Two students are ...
The Ancient Heavens: Exploring the History of Astronomy
... these activities help participants appreciate not only what we know, but how we know it. ...
... these activities help participants appreciate not only what we know, but how we know it. ...
PP 23-The Solar System
... The sun is nearly all hydrogen and helium, with traces (less than 2% by mass in total) of elements with heavier nuclei. ...
... The sun is nearly all hydrogen and helium, with traces (less than 2% by mass in total) of elements with heavier nuclei. ...
PTYS/ASTR 206 – Section 2 - Lunar and Planetary Laboratory
... Thus, using this to answer the questions, we get: (a) the stars that have a longer wavelength of maximum emission than the Sun are: Epsilon Indi, Tau Ceti, Epsilon Eridani, and Lalande 21185. The stars that have a shorter maximum wavelength of emission than the Sun are Altair and Procyon (b) the sta ...
... Thus, using this to answer the questions, we get: (a) the stars that have a longer wavelength of maximum emission than the Sun are: Epsilon Indi, Tau Ceti, Epsilon Eridani, and Lalande 21185. The stars that have a shorter maximum wavelength of emission than the Sun are Altair and Procyon (b) the sta ...
Hitomi Observation of the Highly Obscured High-Mass X-ray
... matter, NIR spectrum is consistent with no systemic velocity of the sgB[e] star (c∆λ/λ=110±130 km/s). Assuming that the line-emitting matter follows the compact object that rotates around a companion with a mass of 30 M⊙ , a distance of 1013 cm, and an inclination angle of 45◦ , the maximum line-of- ...
... matter, NIR spectrum is consistent with no systemic velocity of the sgB[e] star (c∆λ/λ=110±130 km/s). Assuming that the line-emitting matter follows the compact object that rotates around a companion with a mass of 30 M⊙ , a distance of 1013 cm, and an inclination angle of 45◦ , the maximum line-of- ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.