distances
... Measuring a Star’s Motion • A star’s radial motion is determined from the Doppler shift of its spectral lines • The amount of shift depends on the star’s radial velocity • Δλ = the shift in wavelength of an absorption line • λ = resting wavelength, the radial speed v is ...
... Measuring a Star’s Motion • A star’s radial motion is determined from the Doppler shift of its spectral lines • The amount of shift depends on the star’s radial velocity • Δλ = the shift in wavelength of an absorption line • λ = resting wavelength, the radial speed v is ...
Stars - Mike Brotherton
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron ...
... The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 Msun), leading to the formation of an iron ...
White Dwarfs
... 18. Which of the following statements accurately describe some observed properties of type Ia and type II supernovae? a. Type Ia supernovae have hydrogen lines in their spectra. b. Type II supernovae have hydrogen lines in their spectra. c. Type Ia supernovae are more luminous. d. Both a and c above ...
... 18. Which of the following statements accurately describe some observed properties of type Ia and type II supernovae? a. Type Ia supernovae have hydrogen lines in their spectra. b. Type II supernovae have hydrogen lines in their spectra. c. Type Ia supernovae are more luminous. d. Both a and c above ...
Slide 1
... growth indicates the Earth's climatic environment over time • Unlike the other types of supernovae, Type Ia supernovae are generally found in all types of galaxies, including ellipticals. ...
... growth indicates the Earth's climatic environment over time • Unlike the other types of supernovae, Type Ia supernovae are generally found in all types of galaxies, including ellipticals. ...
HERE
... 26. Which gas was not believed to be present on Earth at the time of its formation 4.4 billion years ago? 27. Oxygen was introduced into the atmosphere as a by product of… ...
... 26. Which gas was not believed to be present on Earth at the time of its formation 4.4 billion years ago? 27. Oxygen was introduced into the atmosphere as a by product of… ...
A Story about a Star`s Life
... may appear dim because it is very far away or it does not emit much energy ...
... may appear dim because it is very far away or it does not emit much energy ...
Stars and Galaxies part 3
... • (Red) Giants and Supergiants – generally much larger than main sequence stars ...
... • (Red) Giants and Supergiants – generally much larger than main sequence stars ...
Teacher`s Guide Understanding: The Universe
... What is significant about the redshifted spectra of galaxies? (The redshift in the spectra of galaxies implies that they are moving away from one another, and that could mean that the universe is expanding.) ...
... What is significant about the redshifted spectra of galaxies? (The redshift in the spectra of galaxies implies that they are moving away from one another, and that could mean that the universe is expanding.) ...
pdf of paper
... protons. Amazingly enough, another heliwn nucleus collides \\ith this shortlived target, leading to the formation of carbon. The process would seem about as likely as crossing a stream by stepping fleetingly on a log. A delicate match between the energies of helium, the unstable berylJium and the re ...
... protons. Amazingly enough, another heliwn nucleus collides \\ith this shortlived target, leading to the formation of carbon. The process would seem about as likely as crossing a stream by stepping fleetingly on a log. A delicate match between the energies of helium, the unstable berylJium and the re ...
HW #4 (due March 27)
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
TYPES OF STARS
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
... When astronomers look through their telescopes, they see billions of stars. What can they learn from their observations? In class, we’ve learned that the shape of the spectrum (especially, the wavelength at which it reaches its maximum intensity) can be used to determine a star’s temperature. In add ...
Stellar Structure - Astronomy Centre
... (see blackboard) • Is a star solid, liquid or gaseous? • Mean density and surface temperature (see blackboard) ...
... (see blackboard) • Is a star solid, liquid or gaseous? • Mean density and surface temperature (see blackboard) ...
Back ground information
... Visible light has more energy and smaller wavelengths than infrared radiation and is divided into the different colors humans see. Moving from longer wavelengths (less energy) to shorter wavelengths (more energy) one finds red, orange, yellow, green, blue, and violet. The color of the light emitted ...
... Visible light has more energy and smaller wavelengths than infrared radiation and is divided into the different colors humans see. Moving from longer wavelengths (less energy) to shorter wavelengths (more energy) one finds red, orange, yellow, green, blue, and violet. The color of the light emitted ...
Stellar and Atomic Spectra
... • Because each element has it own unique pattern of spectral lines, the spectral lines from stars can be used to determine the composition, or the relative number of atoms of each elements, of the stars ...
... • Because each element has it own unique pattern of spectral lines, the spectral lines from stars can be used to determine the composition, or the relative number of atoms of each elements, of the stars ...
PHYS299B_Final_HudsonJustin
... same time getting twice the data. With this we can ass to the AAVSO¹ data base. ...
... same time getting twice the data. With this we can ass to the AAVSO¹ data base. ...
Extragalactic AO Science
... AO systems produce additional background in Near-IR and reduce throughput further making it difficult to observe faint extended sources. Normal galaxy disks only achieve a maximum SB of K~16 mag/sq arcsec and this fades as (1+z)4. This means all normal disks are fainter than 22.5 mag within 0.05x0.0 ...
... AO systems produce additional background in Near-IR and reduce throughput further making it difficult to observe faint extended sources. Normal galaxy disks only achieve a maximum SB of K~16 mag/sq arcsec and this fades as (1+z)4. This means all normal disks are fainter than 22.5 mag within 0.05x0.0 ...
Lec10_2D
... The Death of a High Mass Star When the star’s core turns to iron, it again collapses. The increased pressure and temperature then causes iron to fuse. However… The products of iron fusion weigh more than the initial iron nucleus. According to E = m c2, this means that iron fusion does not make ener ...
... The Death of a High Mass Star When the star’s core turns to iron, it again collapses. The increased pressure and temperature then causes iron to fuse. However… The products of iron fusion weigh more than the initial iron nucleus. According to E = m c2, this means that iron fusion does not make ener ...
The Sun - Center for Astrophysics and Space Astronomy CASA
... a ball of electrons will radiate photons. These elusive particles carry away 99.9% of the energy. So poorly coupled to regular matter that they travel unimpeded through the Universe at close to the speed of light. ...
... a ball of electrons will radiate photons. These elusive particles carry away 99.9% of the energy. So poorly coupled to regular matter that they travel unimpeded through the Universe at close to the speed of light. ...
20.1 A Solar System is Born
... Upsetting the Balance “As the matter in a globule collapses… inward the temperature… increases and the stage is set for stars to form.” Solar nebula – the cloud of gas and dust that formed our solar system. ...
... Upsetting the Balance “As the matter in a globule collapses… inward the temperature… increases and the stage is set for stars to form.” Solar nebula – the cloud of gas and dust that formed our solar system. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.