Stellar Lives (continued). Galaxies.
... The Origin of Elements How do we know that elements are produced inside stars? If massive stars do produce heavy elements and disperse them in space, then the total amount of heavy elements should gradually increase with time. We should expect stars born recently to contain more heavy elements than ...
... The Origin of Elements How do we know that elements are produced inside stars? If massive stars do produce heavy elements and disperse them in space, then the total amount of heavy elements should gradually increase with time. We should expect stars born recently to contain more heavy elements than ...
The Big Bang
... Galaxies “Here and Now” Large “modern day” galaxies (those with the smallest lookback times) are usually observed to be regular systems that don’t look particularly disturbed. Most of the small “modern day” galaxies look quite irregular. In very rough numbers, “large” galaxies have 10 billion stars ...
... Galaxies “Here and Now” Large “modern day” galaxies (those with the smallest lookback times) are usually observed to be regular systems that don’t look particularly disturbed. Most of the small “modern day” galaxies look quite irregular. In very rough numbers, “large” galaxies have 10 billion stars ...
Active Galactic Nuclei: are they important?
... Hopkins and Elvis 2009, simulation of the ISM cloud interaction with a hot AGN wind. Even weak wind can lead to cloud dispersion and suppression of potential ...
... Hopkins and Elvis 2009, simulation of the ISM cloud interaction with a hot AGN wind. Even weak wind can lead to cloud dispersion and suppression of potential ...
1.1 Fundamental Observers
... spectra of astronomical sources and measure the wavelength(s) of welldefined spectral feature(s), such as emission or absorption lines (see Figure 1.6). Colours are not sufficient, normally, because stars and galaxies can appear red because they are cool, or because their light is reddened by inters ...
... spectra of astronomical sources and measure the wavelength(s) of welldefined spectral feature(s), such as emission or absorption lines (see Figure 1.6). Colours are not sufficient, normally, because stars and galaxies can appear red because they are cool, or because their light is reddened by inters ...
What is a Red Shift?
... Shifts / Big Bang Theory Who discovered that the Milky Way is not the only galaxy in our Universe? ...
... Shifts / Big Bang Theory Who discovered that the Milky Way is not the only galaxy in our Universe? ...
Earth_Universe04
... • Measuring a star's distance can be very difficult • Stellar parallax • Used for measuring distance to a star • Apparent shift in a star's position due to the orbital motion of Earth • Measured as an angle ...
... • Measuring a star's distance can be very difficult • Stellar parallax • Used for measuring distance to a star • Apparent shift in a star's position due to the orbital motion of Earth • Measured as an angle ...
Kroupa - SatelliteGa.. - University of Hertfordshire
... were not where they should be. “There is something odd about their distribution”, explains Professor Kroupa. “They should be uniformly arranged around the Milky Way, but this is not what we found.” The astronomers discovered that the eleven brightest of the dwarf galaxies lie more or less in the ...
... were not where they should be. “There is something odd about their distribution”, explains Professor Kroupa. “They should be uniformly arranged around the Milky Way, but this is not what we found.” The astronomers discovered that the eleven brightest of the dwarf galaxies lie more or less in the ...
Problem 4: magnitude of the star?
... E. The change in size of the star cannot be determined __C___15. The Milky Way galaxy has a bulge and disk characterstic of spiral galaxies. These features are most plainly seen in images taken in A. Visible light B. Ultraviolet light C. Infrared light D. 21cm radio observations E. X-rays __D___16. ...
... E. The change in size of the star cannot be determined __C___15. The Milky Way galaxy has a bulge and disk characterstic of spiral galaxies. These features are most plainly seen in images taken in A. Visible light B. Ultraviolet light C. Infrared light D. 21cm radio observations E. X-rays __D___16. ...
not - ISDC
... (master thesis on X-ray astronomy) 1996 ● PhD in astrophysics at Hamburg Observatory and at Osservatorio Astronomico di Brera (Milan/Italy) - studying the evolution of distant galaxies (Luminosity Function of BL Lac objects and Seyfert 2 galaxies) 2001 ● 2001-2003: working in Geneva (Switzerland) on ...
... (master thesis on X-ray astronomy) 1996 ● PhD in astrophysics at Hamburg Observatory and at Osservatorio Astronomico di Brera (Milan/Italy) - studying the evolution of distant galaxies (Luminosity Function of BL Lac objects and Seyfert 2 galaxies) 2001 ● 2001-2003: working in Geneva (Switzerland) on ...
ASTR100 Class 01 - University of Maryland Department of
... C. The temperature starts low and ends high in both the raisin cake and the universe. D. The raisins stay roughly the same size as the cake expands, just as galaxies stay roughly the same size as the universe expands. E. The average distance increases with time both between raisins in the cake and b ...
... C. The temperature starts low and ends high in both the raisin cake and the universe. D. The raisins stay roughly the same size as the cake expands, just as galaxies stay roughly the same size as the universe expands. E. The average distance increases with time both between raisins in the cake and b ...
Astronomy - Shelbyville Central Schools
... Stars differ in composition, age, and size. *young stars are rich in hydrogen *older stars use up hydrogen to produce more helium ...
... Stars differ in composition, age, and size. *young stars are rich in hydrogen *older stars use up hydrogen to produce more helium ...
Introduction to Galaxies - West Jefferson Local Schools
... • orbits of stars and gas are “circular”, rotating about disk axis • star formation is on-going; it is can be fairly constant over the age of the galaxy • gas and dust mass fraction is roughly 10-50% of full disk • due on-going star formation, ages of stars widely range from age of galaxy to new • s ...
... • orbits of stars and gas are “circular”, rotating about disk axis • star formation is on-going; it is can be fairly constant over the age of the galaxy • gas and dust mass fraction is roughly 10-50% of full disk • due on-going star formation, ages of stars widely range from age of galaxy to new • s ...
main characteristics of the emission from elliptical galaxies
... In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is because their light is mainly brought by two dierent components: optical radiation ar ...
... In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is because their light is mainly brought by two dierent components: optical radiation ar ...
File
... • Radio Waves - are used with huge telescopes to learn about the structure, composition, and motion of objects in space ...
... • Radio Waves - are used with huge telescopes to learn about the structure, composition, and motion of objects in space ...
File
... in the galaxy that we can’t see (not stars). This is dark matter. The dark matter comprises about 90% of the galaxy’s mass. Dark matter is made of… Active Galaxies ...
... in the galaxy that we can’t see (not stars). This is dark matter. The dark matter comprises about 90% of the galaxy’s mass. Dark matter is made of… Active Galaxies ...
Name
... 40. ______________________ is the attractive force that exists between any two objects in the Universe. The gravitational force is proportional to the square of the distance between their ...
... 40. ______________________ is the attractive force that exists between any two objects in the Universe. The gravitational force is proportional to the square of the distance between their ...
Hubble Deep Field
The Hubble Deep Field (HDF) is an image of a small region in the constellation Ursa Major, constructed from a series of observations by the Hubble Space Telescope. It covers an area 2.5 arcminutes across, about one 24-millionth of the whole sky, which is equivalent in angular size to a 65 mm tennis ball at a distance of 100 metres. The image was assembled from 342 separate exposures taken with the Space Telescope's Wide Field and Planetary Camera 2 over ten consecutive days between December 18 and December 28, 1995.The field is so small that only a few foreground stars in the Milky Way lie within it; thus, almost all of the 3,000 objects in the image are galaxies, some of which are among the youngest and most distant known. By revealing such large numbers of very young galaxies, the HDF has become a landmark image in the study of the early universe, with the associated scientific paper having received over 900 citations by the end of 2014.Three years after the HDF observations were taken, a region in the south celestial hemisphere was imaged in a similar way and named the Hubble Deep Field South. The similarities between the two regions strengthened the belief that the universe is uniform over large scales and that the Earth occupies a typical region in the Universe (the cosmological principle). A wider but shallower survey was also made as part of the Great Observatories Origins Deep Survey. In 2004 a deeper image, known as the Hubble Ultra-Deep Field (HUDF), was constructed from a few months of light exposure. The HUDF image was at the time the most sensitive astronomical image ever made at visible wavelengths, and it remained so until the Hubble Extreme Deep Field (XDF) was released in 2012.