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- Part A What was the distance between the points that would someday become, respectively, the center of the Milky Way Galaxy and the center of the Virgo Cluster at the time of decoupling? (The present separation is 18 Mpc.) Express your answer using two significant figures. 1ΨΕΙ ΑΣΦ ? Request Aswer Submit kpeUsing MBH = 6.6 × 10 Mo, calculate the below. a. Find radius of the Schwarzschild sphere (Schwarzschild radius Rs). You can calculated from the appropriate formula or just use the fact that for an object of 1 solar mass Rs = 3 km. b. Express Rs in km, in AU, in parsecs. c. Using the distance to M87 and your result above, find angular radius of the SMBH (Schwarzschild radius). Express it in arcseconds (") and micro- arcseconds (pas) d. Take the radius of Pluto's orbit equal to 40 AU and find its angular size (in micro-arcseconds, pas) at the distance of M87.The Tully-Fischer method relies on being able to relate the mass of a galaxy to its rotation velocity. Stars in the outer-most regions of the Milky Way galaxy, located at a distance of 50 kpc from the galactic centre, are observed to orbit at a speed vrot determine the mass in the Milky Way that lies interior to 50 kpc. Express your answer in units of the Solar mass. 250 km s-1. Using Kepler's 3rd Law,
- The Kormendy relation for ellipticals can be written as He = 20.2+ 3.0 log R. where R. is the half-light radius (in kpc) and 4e is the surface brightness (in magnitudes per square arc second) at R.. An elliptical galaxy obeying this relation will have a total luminosity Lo R for some index 7. What is the correct value of n? O a. n=-6/5 O b. n= 4/5 T23D Oc n= 16/5 O d. n cannot be determined with the information we have.Closest stars to earth I'm looking for some research papers on the same subject . Could you helpApparent size of Andromeda Galaxy (M31) Imagine the Milky Way Galaxy is a "pizza" and it has a diameter of 30 cm. On this scale, what would be the diameter of the M31 and how far (in cm) is it from the Milky Way? What will be the angular diameter of M31 as viewed from the Milky Way? How many full Moon does M31 span? (You may assume M31 has a face-on view towards us. It has a diameter of 200,000 light years, and at a distance of 2.5 million light year from Earth.)
- As we discussed, clouds are made of a great many small drops. Really - a great many. Imagine a liquid cloud that fills a volume of 1 km3. The clouds contains 100 drops per cubic centimeter; for the sake of argument assume that each is 10 microns (micrometers) in radius. A. How many drops does the cloud contain? Compare this to a big number - say, the number of stars in the galaxy. B. What mass of water does the cloud contain? Compare this to something big - elephants, trucks, that sort of thing. C. What fraction of the cloud volume is filled with condensed water? One way to approach this is to compare the density of the suspended liquid water to the density of the surrounding air. D. How many 1 mm drizzle drops could you make from all the cloud drops? E. How much energy was released when this water condensed from vapor to liquid? If the water condensed in 20 minutes (a reasonable lifetime for a small cloud), what was the (energy per time)? powerPlease do not give solution in image formate thanku Q: You’ve just discovered another new X-ray binary, which we will call Hyp-X2 (“Hyp” for hypothetical). The system Hyp-X2 contains a bright, G2 main-sequence star orbiting an unseen companion. The separation of the stars is estimated to be 12 million kilometers, and the orbital period of the visible star is 5 days. Use Newton’s version of Kepler’s third law to calculate the sum of the masses of the two stars in the system. a)Express your answer in kilograms to two significant figures. b) Give your answer from the previous part in solar masses. ( Msun= 2.0 x 10 /30 kg). Express your answer as a multiple of sun’s mass to two significant figures. C) Determine the mass of the unseen companion. ( Hint: A G2 main-sequence star has a mass of 1 Msun.) Express your answer as a multiple of sun’s mass to two significant figures. The previous answer was not correct, please help meTrue or False 8. Almost all stars are in binary systems. The book says: "So far you have been considering the deaths of stars as if they were all single objects that never interact, but more than half of all stars are members of binary star systems."From this, I would not necessarily say that almost all stars are in binary systems based on this alone, but some other information I am finding says up to 85%. However, the numbers seem to be all over the map outside the course material, and I can not find a solid figure in it from what I have looked at. If it helps, Stars and Galaxies, 10th Edition by Seeds and Beckman is my reference material.
- Observed angular diameters: Crab Nebula- 366.146 arcsecs - distance to Earth = 6,523 light years Orion Nebula- 147.158 arcsecs - distance to Earth = 1,344 light years A) Calculate the linear width for each nebula above. B) Find the percent error for each nebula above.The figure below shows the spectra of two galaxies A and B. Please can i get help with this questions below: 1. Which of these galaxies has ongoing star formation? How can you tell?2. One of these galaxies has Hubble type E3 while the other is SBb. Which is which? What does the 3 inE3 tell you about the galaxy? What does the SB in SBb tell you about the galaxy?3. What effects would dust have on the two spectra?4. Which galaxy would you expect to have more far-infrared emission? ExplYou can estimate the age of the planetary nebula in image (c) in Figure 22.18. The diameter of the nebula is 600 times the diameter of our own solar system, or about 0.8 light-year. The gas is expanding away from the star at a rate of about 25 mi/s. Considering that distance=velocitytime , calculate how long ago the gas left the star if its speed has been constant the whole time. Make sure you use consistent units for time, speed, and distance. Figure 22.18 Gallery of Planetary Nebulae. This series of beautiful images depicting some intriguing planetary nebulae highlights the capabilities of the Hubble Space Telescope. (a) Perhaps the best known planetary nebula is the Ring Nebula (M57), located about 2000 lightyears away in the constellation of Lyra. The ring is about 1 light-year in diameter, and the central star has a temperature of about 120,000 °C. Careful study of this image has shown scientists that, instead of looking at a spherical shell around this dying star, we may be looking down the barrel of a tube or cone. The blue region shows emission from very hot helium, which is located very close to the star; the red region isolates emission from ionized nitrogen, which is radiated by the coolest gas farthest from the star; and the green region represents oxygen emission, which is produced at intermediate temperatures and is at an intermediate distance from the star. (b) This planetary nebula, M2-9, is an example of a butterfly nebula. The central star (which is part of a binary system) has ejected mass preferentially in two opposite directions. In other images, a disk, perpendicular to the two long streams of gas, can be seen around the two stars in the middle. The stellar outburst that resulted in the expulsion of matter occurred about 1200 years ago. Neutral oxygen is shown in red, once-ionized nitrogen in green, and twice-ionized oxygen in blue. The planetary nebula is about 2100 light-years away in the constellation of Ophiuchus. (c) In this image of the planetary nebula NGC 6751, the blue regions mark the hottest gas, which forms a ring around the central star. The orange and red regions show the locations of cooler gas. The origin of these cool streamers is not known, but their shapes indicate that they are affected by radiation and stellar winds from the hot star at the center. The temperature of the star is about 140,000 °C. The diameter of the nebula is about 600 times larger than the diameter of our solar system. The nebula is about 6500 light-years away in the constellation of Aquila. (d) This image of the planetary nebula NGC 7027 shows several stages of mass loss. The faint blue concentric shells surrounding the central region identify the mass that was shed slowly from the surface of the star when it became a red giant. Somewhat later, the remaining outer layers were ejected but not in a spherically symmetric way. The dense clouds formed by this late ejection produce the bright inner regions. The hot central star can be seen faintly near the center of the nebulosity. NGC 7027 is about 3000 light-years away in the direction of the constellation of Cygnus. (credit a: modification of work by NASA, ESA, and the Hubble Heritage (STScI/AURA)-ESA/Hubble Collaboration; credit b: modification of work by Bruce Balick (University of Washington), Vincent Icke (Leiden University, The Netherlands), Garrelt Mellema (Stockholm University), and NASA; credit c: modification of work by NASA, The Hubble Heritage Team (STScI/AURA); credit d: modification of work by H. Bond (STScI) and NASA)
