21ST CENTURY ASTR.:STARS..(LL)-PACKAGE
6th Edition
ISBN: 9780393448450
Author: Kay
Publisher: NORTON
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Chapter 19, Problem 26QP
To determine
By relating the size of a typical AGN with the size of a solar system, how astronomers define the size of an AGN.
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suppose a planetary nebula is 2.8 pc in diameter, and doppler shifts in its spectrum show that the planetary nebula is 33 km/s. how old is the planetary nebula? 1 pc= 3.1 ×10^13 km and 1 yr= 3.2 × 10^7s
Chapter 19 Solutions
21ST CENTURY ASTR.:STARS..(LL)-PACKAGE
Ch. 19.1 - Prob. 19.1ACYUCh. 19.1 - Prob. 19.1BCYUCh. 19.2 - Prob. 19.2CYUCh. 19.3 - Prob. 19.3CYUCh. 19.4 - Prob. 19.4CYUCh. 19 - Prob. 1QPCh. 19 - Prob. 2QPCh. 19 - Prob. 3QPCh. 19 - Prob. 4QPCh. 19 - Prob. 5QP
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- A planetary nebula expanded in radius 0.3 arc seconds in 30 years. Doppler measurements show the nebula is expanding at a rate of 35 km/s. How far away is the nebula in parsecs? First, determine what distance the nebular expanded in parsecs during the time mentioned. Δd = vpc/sTs So we first need to convert the rate into pc/s and the time into seconds: vpc/s = vkm/s (1 pc / 3.09 x 1013km) vpc/s = ? Ts = (Tyr)(365 days/yr)(24 hrs/day)(3600 s/hr) Ts = ? s Δd= vpc/sTs Therefore, Δd = ? pcarrow_forwardWhite Dwarf Size II. The white dwarf, Sirius B, contains 0.98 solar mass, and its density is about 2 x 106 g/cm?. Find the radius of the white dwarf in km to three significant digits. (Hint: Density = mass/volume, and the volume of a 4 sphere is Tr.) 3 km Compare your answer with the radii of the planets listed in the Table A-10. Which planet is this white dwarf is closely equal to in size? I Table A-10 I Properties of the Planets ORBITAL PROPERTIES Semimajor Axis (a) Orbital Period (P) Average Orbital Velocity (km/s) Orbital Inclination Planet (AU) (106 km) (v) (days) Eccentricity to Ecliptic Mercury 0.387 57.9 0.241 88.0 47.9 0.206 7.0° Venus 0.723 108 0.615 224.7 35.0 0.007 3.4° Earth 1.00 150 1.00 365.3 29.8 0.017 Mars 1.52 228 1.88 687.0 24.1 0.093 1.8° Jupiter 5.20 779 11.9 4332 13.1 0.049 1.30 Saturn 9.58 1433 29.5 10,759 9.7 0.056 2.5° 30,799 60,190 Uranus 19.23 2877 84.3 6.8 0.044 0.8° Neptune * By definition. 30.10 4503 164.8 5.4 0.011 1.8° PHYSICAL PROPERTIES (Earth = e)…arrow_forwardH5. A star with mass 1.05 M has a luminosity of 4.49 × 1026 W and effective temperature of 5700 K. It dims to 4.42 × 1026 W every 1.39 Earth days due to a transiting exoplanet. The duration of the transit reveals that the exoplanet orbits at a distance of 0.0617 AU. Based on this information, calculate the radius of the planet (expressed in Jupiter radii) and the minimum inclination of its orbit to our line of sight. Follow up observations of the star in part reveal that a spectral feature with a rest wavelength of 656 nm is redshifted by 1.41×10−3 nm with the same period as the observed transit. Assuming a circular orbit what can be inferred about the planet’s mass (expressed in Jupiter masses)?arrow_forward
- For a main sequence star with luminosity L, how many kilograms of hydrogen is being converted into helium per second? Use the formula that you derive to estimate the mass of hydrogen atoms that are converted into helium in the interior of the sun (LSun = 3.9 x 1026 W). (Note: the mass of a hydrogen atom is 1 mproton and the mass of a helium atom is 3.97 mproton. You need four hydrogen nuclei to form one helium nucleus.)arrow_forward1. The neutrino flux from SN 1987A was estimated to be 1.3 x 1014 m-2 at the location of Earth. If the average energy per neutrino was approximately 4.2 MeV, estimate the total amount of energy in joules released via neutrinos during the supernova explosion. (SN 1987A was located in the LMC at a distance of 50 kpc.).arrow_forwardWhat is the ratio of the percent of metals in extreme Population I stars (3%) to that in extreme Population II stars (0.05%)? NpopI NpopII =arrow_forward
- As a cluster of stars begins to age, which type of star in the cluster will move off the main sequence of the H-R diagram first? 1) all the stars in a cluster are born at the same time; so they will all move off the main sequence at the same time, as they evolve 2) G type stars, like our Sun 3) M type stars, which are the coolest 4) the lowest mass stars, which have the least amount of fuel for fusion 5) the O and B type starsarrow_forwardHow much energy would be released if a star with a mass of 25 Msun and a radius of 10 Rsun detonates as a supernova explosion in 1 second? (Hint: think about the definition of binding energy). Express your answer in terms of solar luminosities.arrow_forwardthe co te on Pictor. The 270 TOI System TOI 270 c Earth 365-day orbit $1 AU from Sun Habitable 5.7-day orbit 0.05 AU $2.4 Earth radii Largest in system 59 F, 15 C 300 F, 150 C TOI 270 TOI 270 d M3-type dwarf star TOI 270 b $11.4-day orbit 0.07 AU 3.4-day orbit 2.1 Earth radii 0.03 AU Temperate 1.25 Earth radii Likely rocky 150 F. 67 C 490 F. 254 C Figure taken from https://exoplanets.nasa.gov/news/1593/tess-scores-hat-trick-with-3-new-worlds/ What makes the TOI-270 system particularly interesting is that the three exoplanets detected this far (there may be more) have sizes comparable to the Earth. Compare the orbital period of TOI 270 c and TOI 270 d. For every revolution that TOI 270 d makes around the host star TOI 270, how many revolutions does TOI 270 c make?arrow_forward
- The place on the H–R diagram where contracting protostars first become visible is a. the horizontal branch. b. the instability strip. c. the birth line. d. the zero-age main sequence. e. none of the above.arrow_forward1. A planetary nebula has an angular diameter of 76 arc seconds and a distance of 5100 ly. What is its linear diameter (in ly)? Hint: Use the small-angle formula: angular diameter (in arc seconds) 2.06 ✕ 105 = linear diameter distance 2. Suppose a planetary nebula is 3.2 pc in diameter, and Doppler shifts in its spectrum show that the planetary nebula is expanding at 31 km/s. How old is the planetary nebula in yr? (Note: 1 pc = 3.1 ✕ 1013 km and 1 yr = 3.2 ✕ 107 s.)arrow_forwardPlace the following events in the formation of stars in the proper chronological sequence, with the oldest first and the youngest last. w. the gas and dust in the nebula flatten to a disk shape due to gravity and a steadily increasing rate of angular rotation x. a star emerges when the mass is great enough and the temperature is high enough to trigger thermonuclear fusion in the core y. the rotation of the nebular cloud increases as gas and dust concentrates by gravity within the growing protostar in the center z. some force, perhaps from a nearby supernova, imparts a rotation to a nebular cloud y, then z, then w, then x z, then y, then w, then x w, then y, then z, then x z, then x, then w, then y x, then z, then y, then w MacBook Air on .H. O O O Oarrow_forward
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