galaxy evolution
... What are Quasars? • A Brief History of Quasars • In early 1960s, Maarten Schmidt discovered that the hydrogen emission lines in the visible spectrum of the optical component of radio source 3C 273 was highly redshifted (about 80 nm), which implied a recessional speed of 17% of the speed of light. • ...
... What are Quasars? • A Brief History of Quasars • In early 1960s, Maarten Schmidt discovered that the hydrogen emission lines in the visible spectrum of the optical component of radio source 3C 273 was highly redshifted (about 80 nm), which implied a recessional speed of 17% of the speed of light. • ...
AST301.Ch22.NeutGammBH - University of Texas Astronomy
... its position in the sky more accurately, and then see spectral lines in its optical “afterglow.” The resulting Doppler shift was a redshift and it was enormous. As we’ll see later, because the universe is expanding, redshift can be used to get distance. Resulting distance for this gamma ray burst wa ...
... its position in the sky more accurately, and then see spectral lines in its optical “afterglow.” The resulting Doppler shift was a redshift and it was enormous. As we’ll see later, because the universe is expanding, redshift can be used to get distance. Resulting distance for this gamma ray burst wa ...
Astronomy 1001/1005 Final Exam (250 points)
... You will NOT get your bubble sheet back One page of notes is allowed Use a #2 pencil on the bubble sheet. Make your bubbles dark and neat. There are 50 multiple choice problems and your choice of 5 short answer questions with point values given for each. ...
... You will NOT get your bubble sheet back One page of notes is allowed Use a #2 pencil on the bubble sheet. Make your bubbles dark and neat. There are 50 multiple choice problems and your choice of 5 short answer questions with point values given for each. ...
Brock physics - Brock University
... 47. The electron neutrino (νe ) produced in hydrogen fusion in the core of the Sun can transform into the muon neutrino (νµ ) or tau neutrino (ντ ) as it travels through (a) the Sun’s interior with a high electron density. (b) the free space between the Sun and the Earth. (c) the Earth’s crust on it ...
... 47. The electron neutrino (νe ) produced in hydrogen fusion in the core of the Sun can transform into the muon neutrino (νµ ) or tau neutrino (ντ ) as it travels through (a) the Sun’s interior with a high electron density. (b) the free space between the Sun and the Earth. (c) the Earth’s crust on it ...
Introduction Notes - Sunflower Astronomy
... Low mass stars like our Sun die quietly as white dwarfs while high mass stars die violently through supernovae explosions resulting in neutron stars or black holes. Star Clusters: can form from massive gas clouds. Clusters are of particular interest to astronomers since they reveal most of the infor ...
... Low mass stars like our Sun die quietly as white dwarfs while high mass stars die violently through supernovae explosions resulting in neutron stars or black holes. Star Clusters: can form from massive gas clouds. Clusters are of particular interest to astronomers since they reveal most of the infor ...
Document
... Suppose line of sight is in orbital plane Star has a periodic motion towards and away from Earth – radial velocity varies sinusoidally ...
... Suppose line of sight is in orbital plane Star has a periodic motion towards and away from Earth – radial velocity varies sinusoidally ...
FIRST LIGHT IN THE UNIVERSE
... density of SF since z~3 which accounts for the observed stellar mass density at z=0. Half the stars we see today were formed by z~2. • Galaxy populations identified by various means (sub-mm, LBGs, BzK, DRG..) can be connected by their clustering, intermittent SF and dust content. • The emerging pict ...
... density of SF since z~3 which accounts for the observed stellar mass density at z=0. Half the stars we see today were formed by z~2. • Galaxy populations identified by various means (sub-mm, LBGs, BzK, DRG..) can be connected by their clustering, intermittent SF and dust content. • The emerging pict ...
Distances in Space
... Used to measure the distance between stars and galaxies. c) Proxima Centauri, the next closest star after the Sun, is 4.2 ly away. It takes light 4.2 years to travel that distance. d) ** Remember, Light-year is a distance, not a unit of time. ...
... Used to measure the distance between stars and galaxies. c) Proxima Centauri, the next closest star after the Sun, is 4.2 ly away. It takes light 4.2 years to travel that distance. d) ** Remember, Light-year is a distance, not a unit of time. ...
Molecular Gas in Nearby Dwarf Galaxies:
... Taken together, suggest that what matters in the HIH2 conversion is the amount of matter in the disk (Σ*), not just the amount of “stuff” ...
... Taken together, suggest that what matters in the HIH2 conversion is the amount of matter in the disk (Σ*), not just the amount of “stuff” ...
ASTRONOMY 1 ... You may use this only this study guide for reference... No electronic devises: I pads, lap tops, phones, etc.
... 3. Why don't we see hydrogen Balmer lines in the spectra of very hot stars (like 45,000 K+/-) 4. What is the he proton-proton chain? Why does it need a high temperature? 5. What is a white dwarf? a supergiant star? A main sequence star? What type is our Sun? 6. The sun generates energy by fusion? By ...
... 3. Why don't we see hydrogen Balmer lines in the spectra of very hot stars (like 45,000 K+/-) 4. What is the he proton-proton chain? Why does it need a high temperature? 5. What is a white dwarf? a supergiant star? A main sequence star? What type is our Sun? 6. The sun generates energy by fusion? By ...
Big Bang, 429
... 3. Why don't we see hydrogen Balmer lines in the spectra of very hot stars (like 45,000 K+/-) 4. What is the he proton-proton chain? Why does it need a high temperature? 5. What is a white dwarf? a supergiant star? A main sequence star? What type is our Sun? 6. The sun generates energy by fusion? By ...
... 3. Why don't we see hydrogen Balmer lines in the spectra of very hot stars (like 45,000 K+/-) 4. What is the he proton-proton chain? Why does it need a high temperature? 5. What is a white dwarf? a supergiant star? A main sequence star? What type is our Sun? 6. The sun generates energy by fusion? By ...
Your Star: _____________________ d = 1 / p
... * Normally, we compare the brightness to another (distant) star instead of the Sun, since the Sun is obviously much brighter and closer than other stars. We use the Sun here because we want to use solar units throughout. ...
... * Normally, we compare the brightness to another (distant) star instead of the Sun, since the Sun is obviously much brighter and closer than other stars. We use the Sun here because we want to use solar units throughout. ...
Examples
... We saw earlier how the strength of absorption lines can be related to the chemical abundance of a star, from the Boltzmann and Saha equations However, stars do not have a uniform composition, temperature or density and therefore a proper analysis must account for where in the atmosphere the abso ...
... We saw earlier how the strength of absorption lines can be related to the chemical abundance of a star, from the Boltzmann and Saha equations However, stars do not have a uniform composition, temperature or density and therefore a proper analysis must account for where in the atmosphere the abso ...
What do the stars tell us?
... dwarf must be accreting mass. To explode with no hydrogen spectrum, it must be accreting hydrogen-free material. The most likely source of hydrogen-free material is another white dwarf. Thus SN Ia are all explosions of hydrogen-free white dwarf stars that grow to 1.4 solar masses - this makes the ex ...
... dwarf must be accreting mass. To explode with no hydrogen spectrum, it must be accreting hydrogen-free material. The most likely source of hydrogen-free material is another white dwarf. Thus SN Ia are all explosions of hydrogen-free white dwarf stars that grow to 1.4 solar masses - this makes the ex ...
Earth`s Motions
... in motion is how planets were discovered. The retrograde motion of planets is more easily explained by the heliocentric model rather than the geocentric model. ...
... in motion is how planets were discovered. The retrograde motion of planets is more easily explained by the heliocentric model rather than the geocentric model. ...
pptx - Particle Physics and Particle Astrophysics
... • thermal emission from Galactic dust at 10-30 K • mostly far infra-red and submillimetre • thermal emission from the CMB • submillimetre and microwave • “spinning dust” • 5-30 mm, from very small, rapidly-spinning dust grains (important as foreground to CMB emission) • line emission from gas • 21 c ...
... • thermal emission from Galactic dust at 10-30 K • mostly far infra-red and submillimetre • thermal emission from the CMB • submillimetre and microwave • “spinning dust” • 5-30 mm, from very small, rapidly-spinning dust grains (important as foreground to CMB emission) • line emission from gas • 21 c ...
handout
... i. Brightest stars : _________ magnitude ii. Faintest stars ( _____________ eye): _______ magnitude iii. 1st mag stars appear ____________ times brighter than 6th mag stars iv. larger magnitude => _________________ object! B. The magnitude scale system can be extended toward ____________ numbers (__ ...
... i. Brightest stars : _________ magnitude ii. Faintest stars ( _____________ eye): _______ magnitude iii. 1st mag stars appear ____________ times brighter than 6th mag stars iv. larger magnitude => _________________ object! B. The magnitude scale system can be extended toward ____________ numbers (__ ...
Tunable light emission from a boron nitride nanotube device
... the focus of this research, appear far superior to those of other materials currently being used as light emitters, for example, in applications linked to optical storage (DVD’s...) or communications. Boron nitride is extremely efficient in ultraviolet light emission, one of the best materials curre ...
... the focus of this research, appear far superior to those of other materials currently being used as light emitters, for example, in applications linked to optical storage (DVD’s...) or communications. Boron nitride is extremely efficient in ultraviolet light emission, one of the best materials curre ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.