Chapter 10: Measuring the Stars - Otto
... Binary stars • Most stars are members of multiple-star systems - Binary-star systems (2) most common • Visual binaries (see 2 stars) • Spectroscopic binaries (detect Doppler shift from one or both orbiting stars) • Eclipsing binaries (one passes in front of other, varying light output) ...
... Binary stars • Most stars are members of multiple-star systems - Binary-star systems (2) most common • Visual binaries (see 2 stars) • Spectroscopic binaries (detect Doppler shift from one or both orbiting stars) • Eclipsing binaries (one passes in front of other, varying light output) ...
PLANETS
... • Astrometric detection not yet achieved • As with radial velocity, dependence on orbital inclination, eccentricity • Very promising future: Keck interferometer, Space Interferometry Mission (SIM), ESA mission GAIA, and others • Planned astrometric errors at the ~10 microarcsecond level – good enoug ...
... • Astrometric detection not yet achieved • As with radial velocity, dependence on orbital inclination, eccentricity • Very promising future: Keck interferometer, Space Interferometry Mission (SIM), ESA mission GAIA, and others • Planned astrometric errors at the ~10 microarcsecond level – good enoug ...
PLANETS
... • Astrometric detection not yet achieved • As with radial velocity, dependence on orbital inclination, eccentricity • Very promising future: Keck interferometer, Space Interferometry Mission (SIM), ESA mission GAIA, and others • Planned astrometric errors at the ~10 microarcsecond level – good enoug ...
... • Astrometric detection not yet achieved • As with radial velocity, dependence on orbital inclination, eccentricity • Very promising future: Keck interferometer, Space Interferometry Mission (SIM), ESA mission GAIA, and others • Planned astrometric errors at the ~10 microarcsecond level – good enoug ...
Measuring the Gravity in Stars
... Simply put, you gravity is related to mass and radius (g, M, R). If you measure 2 you have the third and there are a several methods to get the different quantities. ...
... Simply put, you gravity is related to mass and radius (g, M, R). If you measure 2 you have the third and there are a several methods to get the different quantities. ...
AV_Paper1_TheAgeOfTheUniverse
... “Since the beginning of time,” is a hackneyed phrase, attached with some arbitrary subject, that looks to exaggerate any issue its paired with. Although the use of the phrase highlights an individual’s vague grasp on the depth of time and use of uninspired hyperbole, one could find it surprising th ...
... “Since the beginning of time,” is a hackneyed phrase, attached with some arbitrary subject, that looks to exaggerate any issue its paired with. Although the use of the phrase highlights an individual’s vague grasp on the depth of time and use of uninspired hyperbole, one could find it surprising th ...
Supplementary Information
... the limit of a thin and extended disk. The smearing due to the instrumental resolution in the spatial and spectral domains is taken into account by convolving the inclined model with the Gaussian point spread function of the appropriate width. The outputs of each model are full data cubes and veloci ...
... the limit of a thin and extended disk. The smearing due to the instrumental resolution in the spatial and spectral domains is taken into account by convolving the inclined model with the Gaussian point spread function of the appropriate width. The outputs of each model are full data cubes and veloci ...
Section 24.2 Astronomical Tools
... just like a radio antenna, absorbs and transmits these waves to an amplifier. ...
... just like a radio antenna, absorbs and transmits these waves to an amplifier. ...
In the icy near-vacuum of interstellar space are seething
... the cloud during the star's early, formative stages. And yet these tiny grains—of uncertain composition, though graphite, silicon, carbide, and iron are possible constituents—contribute less than one percent to a cloud's total mass. Their effect becomes appreciable only because of the great size of ...
... the cloud during the star's early, formative stages. And yet these tiny grains—of uncertain composition, though graphite, silicon, carbide, and iron are possible constituents—contribute less than one percent to a cloud's total mass. Their effect becomes appreciable only because of the great size of ...
Comments
... Hbeta, Mg_b, & Fe5335) with evolutionary stellar population models to derive lightaveraged ages, metallicities and the element abundance ratios Mg/Fe. We find that all these three stellar parameters of the distant galaxies obey a scaling with velocity dispersion (mass) which is very well consistent ...
... Hbeta, Mg_b, & Fe5335) with evolutionary stellar population models to derive lightaveraged ages, metallicities and the element abundance ratios Mg/Fe. We find that all these three stellar parameters of the distant galaxies obey a scaling with velocity dispersion (mass) which is very well consistent ...
3rd EXAM VERSION A key - Department of Physics and Astronomy
... B. *the apparent motion of jets of gas at speeds faster than light C. the apparent motion of arcs of light caused by gravitational lensing D. the motion of galaxies at redshifts z > 1 24. In the “unified model” of active galaxies, the main difference between quasars, blazers, and radio galaxies appe ...
... B. *the apparent motion of jets of gas at speeds faster than light C. the apparent motion of arcs of light caused by gravitational lensing D. the motion of galaxies at redshifts z > 1 24. In the “unified model” of active galaxies, the main difference between quasars, blazers, and radio galaxies appe ...
HST Key Project to Measure the Hubble Constant from
... exploding white dwarf stars that have reached the 1.4 solar mass white dwarf limit Should have same luminosity because come from stars of same mass that explode in same way Determine true luminosity by using CVs to measure distance to galaxies Confirm L of all WD SNs are about the same BRIGHT: 10 bi ...
... exploding white dwarf stars that have reached the 1.4 solar mass white dwarf limit Should have same luminosity because come from stars of same mass that explode in same way Determine true luminosity by using CVs to measure distance to galaxies Confirm L of all WD SNs are about the same BRIGHT: 10 bi ...
Gravitational redshifts
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
File - Mr. Pelton Science
... • Stars with varying light output allowed astronomers to map the Milky Way, which has a halo, spiral arm, and a massive galactic black hole at its center. ...
... • Stars with varying light output allowed astronomers to map the Milky Way, which has a halo, spiral arm, and a massive galactic black hole at its center. ...
Abundance of Elements
... Synthetic spectra for cool stars were retrieved from the website of the PHOENIX project( http://www.hs.unihamburg.de/EN/For/ThA/phoenix) critical metallicity calibration has now been initiated based on atmospheric modeling of Fe lines using high resolution spectra of bright (mostly early-type)M ...
... Synthetic spectra for cool stars were retrieved from the website of the PHOENIX project( http://www.hs.unihamburg.de/EN/For/ThA/phoenix) critical metallicity calibration has now been initiated based on atmospheric modeling of Fe lines using high resolution spectra of bright (mostly early-type)M ...
Masses are much harder than distance, luminosity, or temperature
... Masses are much harder than distance, luminosity, or temperature • Since we are only ever seeing a point source, it is hard to determine how much mass is contained. – If we could see another nearby object (another star maybe?) we could use the gravity between the objects as a measure of the mass. ...
... Masses are much harder than distance, luminosity, or temperature • Since we are only ever seeing a point source, it is hard to determine how much mass is contained. – If we could see another nearby object (another star maybe?) we could use the gravity between the objects as a measure of the mass. ...
Stellar Evolution: Evolution: Birth, Life, and Death of Stars
... Observing the stars in various stages of their lives, and putting them in a sequence of logical evolution. Making models using computers, using the laws of physics, and accounting the changes in the composition of the stars that occur due to nuclear fusion. Studying the stellar clusters and/or group ...
... Observing the stars in various stages of their lives, and putting them in a sequence of logical evolution. Making models using computers, using the laws of physics, and accounting the changes in the composition of the stars that occur due to nuclear fusion. Studying the stellar clusters and/or group ...
Estimating the mass and star formation rate in galaxies
... Step 5: We can perform an identical analysis to steps 3 and 4 for a field which contains near‐infrared standard stars visible during the night at elevations similar to our science target. A catalogue of near‐infrared standards for the northern hemisphere is available at: ...
... Step 5: We can perform an identical analysis to steps 3 and 4 for a field which contains near‐infrared standard stars visible during the night at elevations similar to our science target. A catalogue of near‐infrared standards for the northern hemisphere is available at: ...
Status of the Hybrid Doppler Wind Lidar (HDWL) Transceiver ACT
... +/- 16 arcsec pointing knowledge (post-processed) ...
... +/- 16 arcsec pointing knowledge (post-processed) ...
Document
... 1) Do not plug in the telescope 2) Sight and focus telescope on distant object (Moon or top of Mt. Diablo) 3) Attach Finderscope 4) Collimate Finderscope (align it with Primary scope) 5) Put telescope in the Polar Home position (pointing at Polaris) 6) Tighten both clamps and do not loosen them unti ...
... 1) Do not plug in the telescope 2) Sight and focus telescope on distant object (Moon or top of Mt. Diablo) 3) Attach Finderscope 4) Collimate Finderscope (align it with Primary scope) 5) Put telescope in the Polar Home position (pointing at Polaris) 6) Tighten both clamps and do not loosen them unti ...
Stars, Galaxies, and the Universe Section 1 Distances to Stars
... Section 1: Characteristics of Stars ...
... Section 1: Characteristics of Stars ...
Milky Way Galaxy
... call spiral galaxies were referred to as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. The breakthrough came in 1924 when Edwin Hubble was able to measure the distance to the “Great Nebula in Andromeda” (M 31, at right) and found ...
... call spiral galaxies were referred to as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. The breakthrough came in 1924 when Edwin Hubble was able to measure the distance to the “Great Nebula in Andromeda” (M 31, at right) and found ...
Integrated Science
... Neutron stars are one of the possible ends for a star. They result from massive stars which have mass greater than 4 to 8 times that of our Sun. After these stars have finished burning their nuclear fuel, they undergo a supernova explosion. This explosion blows off the outer layers of a star into ...
... Neutron stars are one of the possible ends for a star. They result from massive stars which have mass greater than 4 to 8 times that of our Sun. After these stars have finished burning their nuclear fuel, they undergo a supernova explosion. This explosion blows off the outer layers of a star into ...
The Temperature of Stars
... star as seen from the Earth. The apparent magnitude of a star depends on both how much light the star emits and how far the star is from Earth. Absolute magnitude the brightness that a star would have at a distance of 32.6 lightyears from Earth. The brighter a star is, the lower the number of its ab ...
... star as seen from the Earth. The apparent magnitude of a star depends on both how much light the star emits and how far the star is from Earth. Absolute magnitude the brightness that a star would have at a distance of 32.6 lightyears from Earth. The brighter a star is, the lower the number of its ab ...
Planets around Other Stars - Sierra College Astronomy Home Page
... Strength: smaller planets can be detected this way, including, potentially, Earth-size planets © Sierra College Astronomy Department ...
... Strength: smaller planets can be detected this way, including, potentially, Earth-size planets © Sierra College Astronomy Department ...
arXiv:1404.0641v2 [astro
... The fact that more than a third of the planetary systems in the solar vicinity, discovered by ongoing exoplanetary missions, is younger than 3 Gyr is not surprising, because the continuous star formation (SF) in the Galactic disk supplies young stars, and the fraction of hosts younger than 3 Gyr rep ...
... The fact that more than a third of the planetary systems in the solar vicinity, discovered by ongoing exoplanetary missions, is younger than 3 Gyr is not surprising, because the continuous star formation (SF) in the Galactic disk supplies young stars, and the fraction of hosts younger than 3 Gyr rep ...
Space Interferometry Mission
The Space Interferometry Mission, or SIM, also known as SIM Lite (formerly known as SIM PlanetQuest), was a planned space telescope developed by the U.S. National Aeronautics and Space Administration (NASA), in conjunction with contractor Northrop Grumman. One of the main goals of the mission was the hunt for Earth-sized planets orbiting in the habitable zones of nearby stars other than the Sun. SIM was postponed several times and finally cancelled in 2010.In addition to hunting for extrasolar planets, SIM would have helped astronomers construct a map of the Milky Way galaxy. Other important tasks would have included collecting data to help pinpoint stellar masses for specific types of stars, assisting in the determination of the spatial distribution of dark matter in the Milky Way and in the Local Group of galaxies and using the gravitational microlensing effect to measure the mass of stars.The spacecraft would have used optical interferometry to accomplish these and other scientific goals. This technique collects light with multiple mirrors (in SIM's case, two) which is combined to make an interference pattern which can be very precisely measured.The initial contracts for SIM Lite were awarded in 1998, totaling US$200 million. Work on the SIM project required scientists and engineers to move through eight specific new technology milestones, and by November 2006, all eight had been completed.SIM Lite was originally scheduled for a 2005 launch, aboard an Evolved Expendable Launch Vehicle (EELV). As a result of continued budget cuts, the launch date has been pushed back at least five times. NASA has set a preliminary launch date for 2015 and U.S. federal budget documents confirm that a launch date is expected ""no earlier"" than 2015. The budget cuts to SIM Lite are expected to continue through FY 2010. As of February 2007, many of the engineers working on the SIM program had moved on to other areas and projects, and NASA directed the project to allocate its resources toward engineering risk reduction. However, the preliminary budget for NASA for 2008 included zero dollars for SIM.In December 2007, the Congress restored funding for fiscal year 2008 as part of an omnibus appropriations bill which the President later signed. At the same time the Congress directed NASA to move the mission forward to the development phase. In 2009 the project continued its risk reduction work while waiting for the findings and recommendations of the Astronomy and Astrophysics Decadal Survey, Astro2010, performed by the National Academy of Sciences, which would determine the project's future.On 13 August 2010, the Astro2010 Decadal Report was released and did not recommend that NASA continue the development of the SIM Lite Astrometric Observatory. This prompted NASA Astronomy and Physics Director, Jon Morse, to issue a letter on 24 September 2010 to the SIM Lite project manager, informing him that NASA was discontinuing its sponsorship of the SIM Lite mission and directing the project to discontinue Phase B activities immediately or as soon as practical. Accordingly, all SIM Lite activities were closed down by the end of calendar year 2010.