Spectra and the Doppler Effect
... 8. What happens to the pitch of sound as an object moves away (or recedes) from an observer? (the wave is elongated and therefore moving away at lower frequency) ...
... 8. What happens to the pitch of sound as an object moves away (or recedes) from an observer? (the wave is elongated and therefore moving away at lower frequency) ...
astrocoursespring2012lec2-6
... the main sequence. They burn up their nuclear fuel in only millions or tens of millions of years. Stars with lower masses comprise the yellow, orange, and red dwarfs on the lower-right part of the main sequence, where they remain for billions of years. As a star begins to exhaust the hydrogen fuel i ...
... the main sequence. They burn up their nuclear fuel in only millions or tens of millions of years. Stars with lower masses comprise the yellow, orange, and red dwarfs on the lower-right part of the main sequence, where they remain for billions of years. As a star begins to exhaust the hydrogen fuel i ...
powerpoints - Georgia Southern University Astrophysics
... • The elements and their relative abundances are different for Type Ia and Type II remnants because the progenitors are different. Type Ia remnants from white dwarfs - usually show relatively strong Si, S, Ar, Ca, and Fe, and weak O, Ne, and Mg lines; Type II remnants - from massive stars generally ...
... • The elements and their relative abundances are different for Type Ia and Type II remnants because the progenitors are different. Type Ia remnants from white dwarfs - usually show relatively strong Si, S, Ar, Ca, and Fe, and weak O, Ne, and Mg lines; Type II remnants - from massive stars generally ...
Quiz 3 Feedback Electron Jumps in Atoms Emission and absorption
... “You get the temperature of a star by looking to see whether it has emission lines, absorption lines, or a continuous spectrum.” •All stars essentially have absorption lines on a thermal (continuous) spectrum. If there are emission lines, those come from low-density hotter gas above the surface. “Yo ...
... “You get the temperature of a star by looking to see whether it has emission lines, absorption lines, or a continuous spectrum.” •All stars essentially have absorption lines on a thermal (continuous) spectrum. If there are emission lines, those come from low-density hotter gas above the surface. “Yo ...
Stars in Their Youth
... you see in the sky when plotted in this diagram fall into a diagonal band known as the main sequence. What is shown in Fig. 2.1 is a theoretical H–R diagram. An important property of all stars that fall into this band is that they may be regarded as chemically homogeneous, and are converting hydroge ...
... you see in the sky when plotted in this diagram fall into a diagonal band known as the main sequence. What is shown in Fig. 2.1 is a theoretical H–R diagram. An important property of all stars that fall into this band is that they may be regarded as chemically homogeneous, and are converting hydroge ...
High Energy Astrophysics and Transient Science (or, a tale of radio
... The X-rays originate from regions with temperatures >107 K and sizes 10—100 km … … they are accreting neutron stars and stellar mass black holes in X-ray binary systems ...
... The X-rays originate from regions with temperatures >107 K and sizes 10—100 km … … they are accreting neutron stars and stellar mass black holes in X-ray binary systems ...
Star or planet, or what?
... art”. You know good art when you see it, but it is extremely difficult to define. And like poetry and prose, you can easily point to good examples of each, but infrequently one comes across something that is neither one thing nor the other. The zoological approach leans heavily of the work of Martin ...
... art”. You know good art when you see it, but it is extremely difficult to define. And like poetry and prose, you can easily point to good examples of each, but infrequently one comes across something that is neither one thing nor the other. The zoological approach leans heavily of the work of Martin ...
talk
... While CO, HI, and tracers of star formation (H, FIR) are spatially correlated, their intensities are not. At small scales, the detailed association breaks down. Possibility: outer disk clouds may be smaller than inner disk ==> different formation mechanisms (lack of spiral arms, ...
... While CO, HI, and tracers of star formation (H, FIR) are spatially correlated, their intensities are not. At small scales, the detailed association breaks down. Possibility: outer disk clouds may be smaller than inner disk ==> different formation mechanisms (lack of spiral arms, ...
Photon Dominated Regions
... H2 rotational lines are thermalized for n>104 cm-3 The I6.2/I11.3 ratio is tracing the UV field allow to determine the [PAH+]/[PAH0] ratio and the UV field ...
... H2 rotational lines are thermalized for n>104 cm-3 The I6.2/I11.3 ratio is tracing the UV field allow to determine the [PAH+]/[PAH0] ratio and the UV field ...
Olber`s Paradox
... So if the universe is infinitely big then the sky should be bright But the sky is dark So the universe is not infinitely big So it should have collapsed ...
... So if the universe is infinitely big then the sky should be bright But the sky is dark So the universe is not infinitely big So it should have collapsed ...
STUDY QUESTIONS #10 The MILKY WAY GALAXY diameter face
... 9. Using the rotation curve above, astronomers have calculated a mass for the whole Galaxy, out to about 50,000 light-year radius where there are no more stars, to be about 2 × 1011 M , yet by measuring light at all wavelengths, they only measure one sixth of that mass (3 × 1010 M ). Using the orbit ...
... 9. Using the rotation curve above, astronomers have calculated a mass for the whole Galaxy, out to about 50,000 light-year radius where there are no more stars, to be about 2 × 1011 M , yet by measuring light at all wavelengths, they only measure one sixth of that mass (3 × 1010 M ). Using the orbit ...
Eyeing the retina nebula
... by eons of interaction between the intense light from the central star and the dense clumps of dust and gas formed in the aftermath of the original explosion. Understanding the nature of these features is important because they have an impact on the stellar cycle of death and rebirth. Stars are fuel ...
... by eons of interaction between the intense light from the central star and the dense clumps of dust and gas formed in the aftermath of the original explosion. Understanding the nature of these features is important because they have an impact on the stellar cycle of death and rebirth. Stars are fuel ...
File
... color index for each star. • In 1913 Henry Norris Russell (U.S.) plotted the absolute magnitude versus the spectral type. • The results were the same, the HertzsprungRussell diagram. ...
... color index for each star. • In 1913 Henry Norris Russell (U.S.) plotted the absolute magnitude versus the spectral type. • The results were the same, the HertzsprungRussell diagram. ...
Ch. 21 notes-1
... Describe how the solar system was formed. Introduction Andromeda Galaxy is the most distant object you can see with your unaided eye. Light travels for 2 million years before reaching your eye. Moving Galaxies To study how and when the universe formed, astronomers use information about how galaxi ...
... Describe how the solar system was formed. Introduction Andromeda Galaxy is the most distant object you can see with your unaided eye. Light travels for 2 million years before reaching your eye. Moving Galaxies To study how and when the universe formed, astronomers use information about how galaxi ...
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.