21st Century Astronomy
6th Edition
ISBN: 9780393428063
Author: Kay
Publisher: NORTON
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 16, Problem 30QP
To determine
The reason for which the astronomers prefer to search for planets around low-mass stars.
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solution
Students have asked these similar questions
Time
From this light curve, we can deduce that...
O the star has a high mass exoplanet orbiting it
O the star has an exoplanet orbiting it that has an eccentric orbit
O the star has an exoplanet orbiting it that has an eccentric orbit
O the star has an exoplanet that is not on the same orbital plane as the star
L
Brightness
(Astronomy)
Binary Pulsar.
Part A: Use the orbital period 27 min for the binary pulsar (two neutron stars orbit each other) to find the orbital separation of the pair in AU and solar radii. Assume a neutron star's mass is 3 solar masses. (Hints: Use the version of Kepler's third law for binary stars.)
Part B: Is this system orbiting closer or further than Mercury is to the Sun?
H5.
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)?
Chapter 16 Solutions
21st Century Astronomy
Ch. 16.1 - Prob. 16.1CYUCh. 16.3 - Prob. 16.3CYUCh. 16.4 - Prob. 16.4CYUCh. 16.5 - Prob. 16.5CYUCh. 16 - Prob. 1QPCh. 16 - Prob. 2QPCh. 16 - Prob. 3QPCh. 16 - Prob. 4QPCh. 16 - Prob. 5QPCh. 16 - Prob. 6QP
Ch. 16 - Prob. 8QPCh. 16 - Prob. 9QPCh. 16 - Prob. 10QPCh. 16 - Prob. 11QPCh. 16 - Prob. 12QPCh. 16 - Prob. 13QPCh. 16 - Prob. 14QPCh. 16 - Prob. 15QPCh. 16 - Prob. 16QPCh. 16 - Prob. 17QPCh. 16 - Prob. 18QPCh. 16 - Prob. 19QPCh. 16 - Prob. 20QPCh. 16 - Prob. 21QPCh. 16 - Prob. 23QPCh. 16 - Prob. 24QPCh. 16 - Prob. 25QPCh. 16 - Prob. 26QPCh. 16 - Prob. 27QPCh. 16 - Prob. 28QPCh. 16 - Prob. 29QPCh. 16 - Prob. 30QPCh. 16 - Prob. 31QPCh. 16 - Prob. 32QPCh. 16 - Prob. 33QPCh. 16 - Prob. 34QPCh. 16 - Prob. 35QPCh. 16 - Prob. 36QPCh. 16 - Prob. 37QPCh. 16 - Prob. 38QPCh. 16 - Prob. 39QPCh. 16 - Prob. 40QPCh. 16 - Prob. 41QPCh. 16 - Prob. 42QPCh. 16 - Prob. 43QPCh. 16 - Prob. 44QPCh. 16 - Prob. 45QP
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Would you expect to find any white dwarfs in the Orion Nebula? (See The Birth of Stars and the Discovery of Planets outside the Solar System to remind yourself of its characteristics.) Why or why not?arrow_forwardIf the Orion Nebula is 8 pc in diameter and has a density of about 6.0 108 hydrogen atoms/m3, what is its total mass? (Notes: The volume of a sphere is 43r3; 1 pc = 3.1 1016 m; the mass of a hydrogen atom is 1.7 1027 kg.)arrow_forwardIf a transit depth of 0.00001 can be detected with the Kepler spacecraft, what is the smallest planet that could be detected around a 0.3 RsunM dwarf star?arrow_forward
- (Astronomy) (Part A) White Dwarf Size II. The white dwarf, Sirius B, contains 0.98 solar mass, and its density is about 2 × 106 g/cm3. Find the radius of the white dwarf in km to three significant digits. (Hint: Density = mass⁄volume, and the volume of a sphere is 4/3πr3). (Part B) 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?arrow_forwardThe microlensing technique for detecting extrasolar planets involves obtaining OBSERVING brightness measurements of a star and identifying brief, periodic dips in its brightness infrared images of a planet with the light from its host star blocked out a spectrum of a star and identifying periodic wavelength shifts in its features brightness measurements of a star and identifying a brief magnification in its brightness a spectrum of an extrasolar planet and identifying elements and compounds present in its atmospherearrow_forwardF2 Planets in the habitable zone of their stars: 1 #3 3 O are so far from their stars that it is very difficult to discover them O are at a temperature where water can exist as a liquid on the planet's surface O are always the planets closest to the star are also called hot Jupiters O cannot exist around stars that are red dwarfs (spectral type M) E G D F3 $ 54 2 4 R F4 LL F DII % 5 Q Search F5 T 9 -0. G < 6 A F6 Y * F7 & 7 H PrtScn U FB 8 Home Jarrow_forward
- Question. Consider a spherical giant molecular cloud, of mass 2e30 kg and radius 3.09e16 m. What is the shortest possible rotation period for this cloud (in years)? Answer. 3.48e4 1.96e2 9.37e7 7.28e6arrow_forwardOne way that astronomers detect planets outside of our solar system (called exoplanets) is commonly referred to as the radial velocity method. This relies on the __________ ___________ to cause shifts in the spectral lines of stars as the stars perform tiny orbits around the center of mass of the host star and its orbiting planets. Those tiny orbits cause the stars to periodically (and therefore predictably) move closer to and further away from our solar system. Luckily, this method only relies on the motion of the star; its physical distance from us does not impact the resulting shifts.arrow_forwardDuring the formation of stars smaller masses may also form and be attracted by a larger mass to become planets Select one: True False CLEAR MY CHOICEarrow_forward
- What is nebulae?arrow_forwardObject Mass Radius Рerson 70 kg 1E-3 km Moon 7E22 kg 1.7E3 km Sun 2E30 kg 7E5 km Earth 6E24 kg GE3 km VY Canis Majoris 3E31 kg IE9 km White Dwarl Star 13 Msun) 6E3 km Neutron Staar 3 Misun 10 km Compute the surlace gravity and escape veloely of each of the objects in the ahove Liblearrow_forwardThe radial velocity method is used to detect exoplanets. The method depends upon the Doppler shift of spectral lines from the star due to the fact that the star and planet both orbit the _______________. Group of answer choices - Black hole - Center of mass - Planet - Stararrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
AstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Glencoe Physics: Principles and Problems, Student...PhysicsISBN:9780078807213Author:Paul W. ZitzewitzPublisher:Glencoe/McGraw-Hill
Foundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
Stars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage Learning
Stars and GalaxiesPhysicsISBN:9781305120785Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax
Glencoe Physics: Principles and Problems, Student...
Physics
ISBN:9780078807213
Author:Paul W. Zitzewitz
Publisher:Glencoe/McGraw-Hill
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Stars and Galaxies
Physics
ISBN:9781305120785
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning