A bowshock model for the wind-ISM interaction of the run
... far side, but expand freely at the near side. From the freely expanding part, we can derive dynamical timescale(s) for the outburst(s) or lower limits for them. The emission in Figure 2 around 10” and below v 110 km s 1 , for instance, fits to an outburst that occurred 13 000 years ago. ...
... far side, but expand freely at the near side. From the freely expanding part, we can derive dynamical timescale(s) for the outburst(s) or lower limits for them. The emission in Figure 2 around 10” and below v 110 km s 1 , for instance, fits to an outburst that occurred 13 000 years ago. ...
슬라이드 1
... Comparison with simulations Protocluster - in qualitative and quantitative agreement : Spatial extent, specific SFR, gas properties, and so on. Quasar - In agreement with with the models of the later phases of massivegalaxy formation when the quasar becomes visible. Unlike for previously described ...
... Comparison with simulations Protocluster - in qualitative and quantitative agreement : Spatial extent, specific SFR, gas properties, and so on. Quasar - In agreement with with the models of the later phases of massivegalaxy formation when the quasar becomes visible. Unlike for previously described ...
Star Types
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
HR Diagram Activity - Mr. Alster`s Science Classes
... Purpose: In this lab we will investigate the relationship between the temperature, brightness and diameter of stars. Introduction The H-R Diagram is a tool that astronomers use to classify stars based on their luminosity, magnitude, temperature, spectral class and evolutionary stage. The H-R Diagram ...
... Purpose: In this lab we will investigate the relationship between the temperature, brightness and diameter of stars. Introduction The H-R Diagram is a tool that astronomers use to classify stars based on their luminosity, magnitude, temperature, spectral class and evolutionary stage. The H-R Diagram ...
LIGO Star Chart
... the northern hemisphere. No telescope is necessary but the sky should be dark. This activity will show you how to locate several features of the night sky. The Big Dipper is the easiest group of stars to identify and can point you in the direction of other interesting areas of the sky. ...
... the northern hemisphere. No telescope is necessary but the sky should be dark. This activity will show you how to locate several features of the night sky. The Big Dipper is the easiest group of stars to identify and can point you in the direction of other interesting areas of the sky. ...
Chapter 17
... showing our own Sun's position and Shapley's distribution of these clusters. 2. Which are more useful in mapping the spiral structure of the Milky Way, H-I or H-II regions? Explain why in terms of the electromagnetic spectrum. 3. William Herschel made the first attempt to map our position in the Mil ...
... showing our own Sun's position and Shapley's distribution of these clusters. 2. Which are more useful in mapping the spiral structure of the Milky Way, H-I or H-II regions? Explain why in terms of the electromagnetic spectrum. 3. William Herschel made the first attempt to map our position in the Mil ...
Stars: Properties and Classification
... made of, what kinds are out there, how they are born, and how they die. Are all stars similar to our Sun? How far away are they? Where did they come from? What do they do? Do they live forever? How do they die? ...
... made of, what kinds are out there, how they are born, and how they die. Are all stars similar to our Sun? How far away are they? Where did they come from? What do they do? Do they live forever? How do they die? ...
GAIA A Stereoscopic Census of our Galaxy - RSSD
... distances to 1% for ~10 million stars to 2.5 kpc distances to 10% for ~100 million stars to 25 kpc rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
... distances to 1% for ~10 million stars to 2.5 kpc distances to 10% for ~100 million stars to 25 kpc rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
The Stars: Distance, Luminosity, Size
... The more massive a Main Sequence star is, the hotter (bluer), and more luminous. The Main Sequence is a mass sequence! ...
... The more massive a Main Sequence star is, the hotter (bluer), and more luminous. The Main Sequence is a mass sequence! ...
Due Date: Thursday, September 21, 2006
... distance between Earth and the star, and D is the diameter of Earth’s orbit around the Sun. That is, D = 2 AU, or approximately 300 million km. Calculate the stellar parallax of the nearest star, Alpha Centauri in degree to see for yourself how difficult it is to measure stellar parallax. The distan ...
... distance between Earth and the star, and D is the diameter of Earth’s orbit around the Sun. That is, D = 2 AU, or approximately 300 million km. Calculate the stellar parallax of the nearest star, Alpha Centauri in degree to see for yourself how difficult it is to measure stellar parallax. The distan ...
Stars and Their Characteristics
... Stars that show variation in brightness are known as variable stars. Distances in space are measured in astronomical units, light-years, and parsecs. Light-Year The distance that light travels in one year, about 9.5 trillion kilometers. Parsec A unit of measurement used to describe distances betwe ...
... Stars that show variation in brightness are known as variable stars. Distances in space are measured in astronomical units, light-years, and parsecs. Light-Year The distance that light travels in one year, about 9.5 trillion kilometers. Parsec A unit of measurement used to describe distances betwe ...
Astron 104 Laboratory #9 Cepheid Variable Stars
... actually radiating into space (i.e, how bright it actually is). • The star’s distance from us. In principle, if we know the first two of these quantities, we can calculate the distance. The apparent magnitude is usually easy to measure because all we need to do is use a telescope that has a calibrat ...
... actually radiating into space (i.e, how bright it actually is). • The star’s distance from us. In principle, if we know the first two of these quantities, we can calculate the distance. The apparent magnitude is usually easy to measure because all we need to do is use a telescope that has a calibrat ...
Lecture Notes – Galaxies
... To measure the mass of a galaxy, we can use the form of Kepler’s 3rd law (for circular orbits), 2 = G M/R to determine the mass (M) inside a star at orbital radius (R), given a rotation velocity Vrot (Vrot ). (M as ∼ 1011 M for our Galaxy.) Plotting V against R gives the rotation curve of the Galax ...
... To measure the mass of a galaxy, we can use the form of Kepler’s 3rd law (for circular orbits), 2 = G M/R to determine the mass (M) inside a star at orbital radius (R), given a rotation velocity Vrot (Vrot ). (M as ∼ 1011 M for our Galaxy.) Plotting V against R gives the rotation curve of the Galax ...
The Milky Way and other Galaxies
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
STARS
... succession of heavier elements • Iron is the most stable; it requires energy verses creating it • Star begins to die ...
... succession of heavier elements • Iron is the most stable; it requires energy verses creating it • Star begins to die ...
GAIA A Stereoscopic Census of our Galaxy
... a large-scale survey of Solar System bodies (~100,000) rare stellar types and rapid evolutionary phases in large numbers support to developments such as JWST, etc. ...
... a large-scale survey of Solar System bodies (~100,000) rare stellar types and rapid evolutionary phases in large numbers support to developments such as JWST, etc. ...
Variable Stars as Essential Astrophysical Tools
... Surveys of new variable stars Locate detached and semi-detached eclipsing binaries in clusters1 Locate contact eclipsing binaries in clusters2 Period/amplitude variations in contact systems3 Period-to-period variability in long period variables Search for cataclysmic variables in clusters4 Search fo ...
... Surveys of new variable stars Locate detached and semi-detached eclipsing binaries in clusters1 Locate contact eclipsing binaries in clusters2 Period/amplitude variations in contact systems3 Period-to-period variability in long period variables Search for cataclysmic variables in clusters4 Search fo ...
HR Diagram of One Solar Mass Evolution
... • After formation white dwarf continues to cool – no energy sources • Coolest “black dwarf” is ~6000K – age of 12 billion years ...
... • After formation white dwarf continues to cool – no energy sources • Coolest “black dwarf” is ~6000K – age of 12 billion years ...
The Milky Way Galaxy
... Radar ranging - good for measuring distances in the solar system (up to about 0.0001 light years) Parallax - good for measuring distances to a few hundred light years ...
... Radar ranging - good for measuring distances in the solar system (up to about 0.0001 light years) Parallax - good for measuring distances to a few hundred light years ...
Electromagnetic spectrum
... becomes visible because it refracts and reflects light from a nearby star A dark nebula is an interstellar molecular cloud whose dust blocks light from stars on the other side of it ...
... becomes visible because it refracts and reflects light from a nearby star A dark nebula is an interstellar molecular cloud whose dust blocks light from stars on the other side of it ...
12 Introduction to Cepheid Variable Stars Exercise
... periods of 25 cepheid variables in the Large and Small Magellanic Clouds. Miss Leavitt noted that when the cepheids were ordered by increasing period that the variable stars were also ordered by increasing brightness. Because both the Small Magellanic Cloud and the Large Magellanic Cloud are each a ...
... periods of 25 cepheid variables in the Large and Small Magellanic Clouds. Miss Leavitt noted that when the cepheids were ordered by increasing period that the variable stars were also ordered by increasing brightness. Because both the Small Magellanic Cloud and the Large Magellanic Cloud are each a ...
20 pm - Starmap
... Many deep sky objects like galaxies and clusters will be within reach. Jupiter satellites and Saturn’s rings will also be visible. A spectacular experience for beginners in astronomy... ...
... Many deep sky objects like galaxies and clusters will be within reach. Jupiter satellites and Saturn’s rings will also be visible. A spectacular experience for beginners in astronomy... ...
Red Giants - Uplift North Hills Prep
... Low mass stars have lifetimes comparable to the Age of the Universe High mass stars have very short lifetimes, and disappear quickly! ...
... Low mass stars have lifetimes comparable to the Age of the Universe High mass stars have very short lifetimes, and disappear quickly! ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.