Goal: To understand how stars form.
... How long do you think this process took to form our sun (and planets)? • It took about 10 million years. A very short time compared to the 4.5 billion years of age that the earth and sun are currently. ...
... How long do you think this process took to form our sun (and planets)? • It took about 10 million years. A very short time compared to the 4.5 billion years of age that the earth and sun are currently. ...
Stimulated Emission and Inversion 9.2.2 Laser Diodes
... tine - we must "pump" the system. Doing this with some other light source providing photons of the only usable energy ∆E = E1 – ∆E = E2 would defeat the purpose of the game; after all that is just the light we want to generate. In semiconductors now, we could inject electrons from some other part of ...
... tine - we must "pump" the system. Doing this with some other light source providing photons of the only usable energy ∆E = E1 – ∆E = E2 would defeat the purpose of the game; after all that is just the light we want to generate. In semiconductors now, we could inject electrons from some other part of ...
Accurate ro-vibrational rest frequencies of DC4H at infrared and
... Context. Diacetylene, C4 H2 , has been identified in several astronomical environments through its infrared spectrum. In contrast, monodeuterated diacetylene (DC4 H) has not been detected in space so far owing to the low isotopic abundance of deuterated species but also to the rather poor laboratory ...
... Context. Diacetylene, C4 H2 , has been identified in several astronomical environments through its infrared spectrum. In contrast, monodeuterated diacetylene (DC4 H) has not been detected in space so far owing to the low isotopic abundance of deuterated species but also to the rather poor laboratory ...
Photometry
... Now you are ready to find the apparent B and V magnitudes. Move to one of the stars indicated on the data sheet on the following page. You may use the monitor / change view button to navigate the area in finder mode. Switch back to photometer / instrument mode before taking your readings. Make sure ...
... Now you are ready to find the apparent B and V magnitudes. Move to one of the stars indicated on the data sheet on the following page. You may use the monitor / change view button to navigate the area in finder mode. Switch back to photometer / instrument mode before taking your readings. Make sure ...
Exercises - Leiden Observatory
... (c) Derive an expression for the maximum central temperature reached by a star of mass M. ...
... (c) Derive an expression for the maximum central temperature reached by a star of mass M. ...
WAVE NATURE OF LIGHT
... planetary orbits around the sun). However, unlike the planetary orbits–which can exist at any distance from the sun–Bohr’s orbits exist only at specific, fixed distances from the nucleus. Bohr called these orbits stationary states. ...
... planetary orbits around the sun). However, unlike the planetary orbits–which can exist at any distance from the sun–Bohr’s orbits exist only at specific, fixed distances from the nucleus. Bohr called these orbits stationary states. ...
The Planetarium Fleischmann Planetarium
... simulations of the ring’s dynamics to estimate the planet’s mass. Kalas and collaborators James R. Graham of the University of California at Berkeley and Mark Clampin of the NASA Goddard Space Flight Center, published their findings in the June 23, 2005 issue of the journal Nature. Fomalhaut, a 200- ...
... simulations of the ring’s dynamics to estimate the planet’s mass. Kalas and collaborators James R. Graham of the University of California at Berkeley and Mark Clampin of the NASA Goddard Space Flight Center, published their findings in the June 23, 2005 issue of the journal Nature. Fomalhaut, a 200- ...
Chemical Signatures in Dwarf Galaxies
... that we see today? Are the dwarf spheroidal and Sloan galaxies that we find in the halo of the MWG related to the gasrich dwarf irregular and gas-poor tran sition galaxies that are further away and often isolated? One way to address these questions is to search for similarities in the chemical patt ...
... that we see today? Are the dwarf spheroidal and Sloan galaxies that we find in the halo of the MWG related to the gasrich dwarf irregular and gas-poor tran sition galaxies that are further away and often isolated? One way to address these questions is to search for similarities in the chemical patt ...
Theory of Massive Star Formation
... • Introduction and observations • Massive star formation models – Fragmentation – Disks and binarity – The radiation pressure problem ...
... • Introduction and observations • Massive star formation models – Fragmentation – Disks and binarity – The radiation pressure problem ...
Lifetime of Stars/ Fusion powers the stars—11 Oct
... • Life time = m(E/m)/L – m (0.007mc2/m)/L – 100Byr – In reality sun uses 10% of fuel. Lifetime is 10Byr 4 1H ...
... • Life time = m(E/m)/L – m (0.007mc2/m)/L – 100Byr – In reality sun uses 10% of fuel. Lifetime is 10Byr 4 1H ...
Chapter 14
... The preceding chapters have traced the story of stars from their birth as clouds of gas in the interstellar medium to their final collapse. This chapter finishes the story by discussing the kinds of objects that remain after a massive star dies. How strange and wonderful that we humans can talk abou ...
... The preceding chapters have traced the story of stars from their birth as clouds of gas in the interstellar medium to their final collapse. This chapter finishes the story by discussing the kinds of objects that remain after a massive star dies. How strange and wonderful that we humans can talk abou ...
Distances and Sizes - University of Iowa Astrophysics
... between the two telescopes (if both of them have to be on Earth – no spacecraft). ...
... between the two telescopes (if both of them have to be on Earth – no spacecraft). ...
Test - Scioly.org
... c. Reflected starlight at optical bands and the planet’s radiation in infrared wavelengths d. Reflected starlight in infrared wavelengths and the planet’s radiation in optical bands 15. Imagine that one of your astronomy “apprentices” is calculating the temperature of a planet that forms from the ...
... c. Reflected starlight at optical bands and the planet’s radiation in infrared wavelengths d. Reflected starlight in infrared wavelengths and the planet’s radiation in optical bands 15. Imagine that one of your astronomy “apprentices” is calculating the temperature of a planet that forms from the ...
Mirrored Image Sep06.pub - High Desert Astronomical Society
... Colorado, and Kathy A. Rages of the SETI Institute, Mountain View, California, created the color composite image from images at three wavelengths in near infrared light obtained with Hubble’s Advanced Camera for Surveys on July 26, 2006. Original Source: Hubble News Release ...
... Colorado, and Kathy A. Rages of the SETI Institute, Mountain View, California, created the color composite image from images at three wavelengths in near infrared light obtained with Hubble’s Advanced Camera for Surveys on July 26, 2006. Original Source: Hubble News Release ...
IB Physics Quantum Physics Schrodinger, Uncertainty Principle, and
... According to the Schrödinger model, the position and the speed of an electron are not well defined. It can be assumed that the uncertainty in the position of the electron in a hydrogen atom is equal to the radius of the electron orbit in the n = 1 state. ...
... According to the Schrödinger model, the position and the speed of an electron are not well defined. It can be assumed that the uncertainty in the position of the electron in a hydrogen atom is equal to the radius of the electron orbit in the n = 1 state. ...
11.3 MB PDF file
... Instrum. 7, 27) at Imperial College in London. Fig. 2 shows a sampie scan obtained with one of the FPs we have used at La Silla. The total scan corresponds to 5.2 A, which is somewhat greater than the free spectral range (distance between overlapping orders) of 4.4 A. Profiles such as this allow us ...
... Instrum. 7, 27) at Imperial College in London. Fig. 2 shows a sampie scan obtained with one of the FPs we have used at La Silla. The total scan corresponds to 5.2 A, which is somewhat greater than the free spectral range (distance between overlapping orders) of 4.4 A. Profiles such as this allow us ...
Is There a Ring Around Milky Way?
... on p/p, are under disruption .and must have been forming a ring structure around our Galaxy. In fact, such satellite-stellar systems may be considered to be the parts of the ring structure around our Galaxy. If the mass and the radius of our Galaxy are 10-15% less than what we have assumed above, we ...
... on p/p, are under disruption .and must have been forming a ring structure around our Galaxy. In fact, such satellite-stellar systems may be considered to be the parts of the ring structure around our Galaxy. If the mass and the radius of our Galaxy are 10-15% less than what we have assumed above, we ...
124-07_Reflection_and_Refraction
... is now on the inside of the glass, not the angle the outside of the glass is hit at) where this happens is given the name critical angle since for any θinc > θcritical, the sine would have to greater than 1. Since this can not be, light must be trapped inside the glass, it must be totally reflected. ...
... is now on the inside of the glass, not the angle the outside of the glass is hit at) where this happens is given the name critical angle since for any θinc > θcritical, the sine would have to greater than 1. Since this can not be, light must be trapped inside the glass, it must be totally reflected. ...
Lab: Heliocentric Parallax
... The computer can simulate a number of different fields (areas on the sky). For this lab, it will randomly select three fields for your use. For each field, you can blink back and forth between 2 virtual photo taken six months apart. As you blink between the photos, you’ll notice several stars shift ...
... The computer can simulate a number of different fields (areas on the sky). For this lab, it will randomly select three fields for your use. For each field, you can blink back and forth between 2 virtual photo taken six months apart. As you blink between the photos, you’ll notice several stars shift ...
An Introduction to Ultraviolet/Visible Molecular Absorption
... narrow settings spectral detail may be lost owing to an increase in the signal-to-noise ratio. In general, it is good practice to narrow slits no more than is necessary for good resolution for the spectrum at hand. D: Instrumentation Instrument Components Instruments used for measuring the absorptio ...
... narrow settings spectral detail may be lost owing to an increase in the signal-to-noise ratio. In general, it is good practice to narrow slits no more than is necessary for good resolution for the spectrum at hand. D: Instrumentation Instrument Components Instruments used for measuring the absorptio ...
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.