Be sure to show work for 4-6- One way that astronomers detect exopla.pdf

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rdzire2014

Be sure to show work for 4-6. One way that astronomers detect exoplanets is by observing the wobble of their host stars via doppler shifts. This is known as the radial velocity technique. The simulated spectra provided on the last page show the position of a 1-solar-mass star's hydrogen-alpha absorption line over time. In the laboratory (at rest), this absorption line occurs 656 nanometers. 4) Calculate the star's radial velocity from each spectrum using the doppler equation, and fill in the table provided. Then, sketch the associated graph. 5) Estimate the period of this system's orbit based on your graph. (Measure the time between two peaks or two troughs.) Convert your answer to years. 6) Calculate the semi-major axis of this exoplanet's orbit using Kepler's law. How does this compare to the orbit of Mercury? (This exoplanet is known as a "hot Jupiter." Does the nickname make sense?) Data Ti.

Education

Line Spectra and Doppler Shifts One way that astronomers detect exoplanets is by observing the wobble of their host stars via doppler shifts. This is known as the radial velocity technique. The simulated spectra provided on the last page show the position of a 1-solar-mass star's hydrogen- alpha absorption line over time. In the laboratory (at rest), this absorption line occurs 656 nanometers. 4) Calculate the star's radial velocity from each spectrum using the doppler equation, and fill in the table provided. Then, sketch the associated graph. 5) Estimate the period of this system's orbit based on your graph. (Measure the time between two peaks or two troughs.) Convert your answer to years. 6) Calculate the semi-major axis of this exoplanet's orbit using Kepler's law. How does this compare to the orbit of Mercury? (This exoplanet is known as a "hot Jupiter." Does the nickname make sense?) Data.

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Sérgio Sacani

Galaxy formation entails the hierarchical assembly of mass, along with the condensation of baryons and the ensuing, selfregulating star formation1,2 . The stars form a collisionless system whose orbit distribution retains dynamical memory that can constrain a galaxy’s formation history3 . The orbits dominated by ordered rotation, with near-maximum circularity λz≈ 1, are called kinematically cold, and the orbits dominated by random motion, with low circularity λz≈ 0, are kinematically hot. The fraction of stars on ‘cold’ orbits, compared with the fraction on ‘hot’ orbits, speaks directly to the quiescence or violence of the galaxies’ formation histories4,5 . Here we present such orbit distributions, derived from stellar kinematic maps through orbit-based modelling for a well-defined, large sample of 300 nearby galaxies. The sample, drawn from the CALIFA survey6, includes the main morphological galaxy types and spans a total stellar mass range from 108.7 to 1011.9 solar masses. Our analysis derives the orbit-circularity distribution as a function of galaxy mass and its volume-averaged total distribution. We find that across most of the considered mass range and across morphological types, there are more stars on ‘warm’ orbits defined as 0.25 ≤λz≤ 0.8 than on either ‘cold’ or ‘hot’ orbits. This orbit-based ‘Hubble diagram’ provides a benchmark for galaxy formation simulations in a cosmological context.

PodHandler.pptx

YashRevankar1

earth_like_planet_presentationtunde akinsanmi

Kepler 432b a_massive_warm_jupiter_in_a_52days_eccentric_orbit_transiting_a_g...

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We present evidence of tidally-driven inspiral in the Kepler-1658 (KOI-4) system, which consists of a giant planet (1.1RJ, 5.9MJ) orbiting an evolved host star (2.9Re, 1.5Me). Using transit timing measurements from Kepler, Palomar/WIRC, and TESS, we show that the orbital period of Kepler-1658b appears to be decreasing at a rate  = - + P 131 22 20 ms yr−1 , corresponding to an infall timescale P P » 2.5 Myr. We consider other explanations for the data including line-of-sight acceleration and orbital precession, but find them to be implausible. The observed period derivative implies a tidal quality factor  ¢ = ´ - + Q 2.50 10 0.62 0.85 4, in good agreement with theoretical predictions for inertial wave dissipation in subgiant stars. Additionally, while it probably cannot explain the entire inspiral rate, a small amount of planetary dissipation could naturally explain the deep optical eclipse observed for the planet via enhanced thermal emission. As the first evolved system with detected inspiral, Kepler-1658 is a new benchmark for understanding tidal physics at the end of the planetary life cycle

LIT 2001 FINAL EXAMPlease respond with a complete, thoughtful an.docx

SHIVA101531

LIT 2001 FINAL EXAM Please respond with a complete, thoughtful answer. Be sure to provide detail by referring to specific examples. DO NOT USE OUTSIDE RESEARCH SOURCES. PART ONE: Answer ONE of the following questions: 1. Describe Langston Hughes’ view of America by tracing at least three of his poems. Also, describe the controversy around the manner in which Hughes portrayed African Americans in his poems. 2. William Carlos Williams uses an “open” style and format and Robert Frost uses a more “constructed”? What are the characteristics of each style – i.e., rhyme, etc. Use examples from their poems. PART TWO: POEM ANALYSIS DO NOT USE OUTSIDE RESEARCH SOURCES. Critically analyze this poem by discussing three major components of analysis: Please read all 7 stanzas of the poem. 1. What are some of the structural elements of the poem? Metaphor, rhyme, symbols, sounds, etc. 2. What does the poem mean? Explain the content of the poem. 3. What is the theme of the poem? To An Athlete Dying Young by A.E.Housman The time you won our town the race We chaired you through the market place; Man and boy stood cheering by, And home we brought you shoulder-high. Today, the road all runners come, Shoulder-high we bring you home, And set you at your threshold down, Townsman of a stiller town. Smart lad, to slip betimes away From fields where glory does not stay, And early though the laurel grows It withers quicker than the rose. Eyes the shady night has shut Cannot see the record cut, And silence sounds no worse than cheers After earth has stopped the ears: Now you will not swell the rout Of lads that wore their honors out, Runners whom renown outran And the name died before the man. So set, before its echoes fade, The fleet foot on the sill of shade, And hold to the low lintel up The still-defended challenge cup. And round that early-laureled head Will flock to gaze the strengthless dead And find unwithered on its curls The garland briefer than a girl’s. Hubble's Law and the Expansion Rate of the Universe This lab is based on the University of Washington’s “Hubble’s Law and the Expansion of the Universe” lab. The website where the images and spectra are located is maintained by the University of Washington Astronomy Department. Learning Objectives Using analyses of images and spectra of selected galaxies, you will 1. measure angular sizes of galaxies and find their distances, 2. measure the redshifts of galaxy spectral lines and find the recessional velocities of the galaxies, 3. create a Hubble Plot to determine a value for Hubble's constant, 4. estimate the age of the Universe from this constant and compare that to the age of the Sun and the Milky Way, 5. and summarize how our view of the Universe has changed as the value of the Hubble constant has improved. Background and Theory In the 1920's, Edwin P. Hubble discovered a relationship, now known as Hubble' ...

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units and measurement xi physics

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In order to use this scheme- Kepler had to have a series of Martian ob.pdf

sidkucheria

In order to use this scheme, Kepler had to have a series of Martian observations 687 days apart, and here Tycho's otserving books provided a veritable gold mine. We can follos this procedure using the same Tyehonic observations that Kepler used; these are found in the following table. For this exercise, graph poper will be used to make it easier to liae up the peotractor. Find the center of the araph paner (the Sgn) and draw a straight ling from the center to the risht hand rdae, parallel to the urid lines. The end of this line represents the basic 00 directice ia space. the direction of the Sun as seen from the Earth at the time of the vemal equinox. Heliocentric longitude is measured from this linc. Draw a circle of 4 cantimeters radius te represent the F.arth's orbit. (Alitough the orbits of Mars and the Earth are actually ellipses, we will see that the circles are pretry good approximations,) Using the protractor centered on the Sun and the vereal cquines as the startine line lav off ceunterclockwise the heliocentric longitudes of the Farth for each date in the table, and label the date. Next with the Earth as the center and with 0 in the direction of and along a line parallel to the vernal squinas. mark off ceuntereleckwise the directions for the scesentric longifudes of Mars, For each pair of observations, the position of Mars in its orbit lies at the imfersection of the lines drawn from both Earth positions through the corresponding goocentric leagitudes of Mars. The nexi step is to determine the center of the circle that will approximate the orbit of Mars. What is needed is the center of the circle which can be determined by taking the perpendicular bisector of three chords of the circle. This method will be discused in class. Dae to constraction errors, these three lines may not all incrsect in one point, so you may have to establish the "best center". The distance from the center to one of Mars' positions will give you the radius of the eircle. Draw the circle representine the orbit of Mars The line from the Sun through the eenter of Mars orbit will lie on the major axis of the oebit of Mars. Derw in the maior avis so. that it wasses threash the Smn. the center of Mars" orbit, and intersets the erbit of Mars. lahel the perihelion and aphelion positions of Mars. Determine the distance Mars is from the Son using the scals that one astronamical unit equals 5 ecatimeters. The eceestricity (c) of the orbit is the ratio of the distanse betwoen the Sun and the center of the orbit for Mars and the semi-major axis of the orbic, measured int the same usits. Determine the eccentrisity (c). PURPOSE: To deternine the orbit of Mars from a limined set of observations. PROCEDURE: Using some of the oboervations of Mans made by Tycho and the method developed by Kepler, an approsimute erbit for the planet Mars will be determined. From our earthbound viewpoint, the eccentricity of Mars ocbit provides the most interesting aspest of the planef's motion. .

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guest8aa6ebb

The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I present the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature.

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