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## Physics 2080; Chapter 29 Part B Notes

by: Amanda Biddlecome

23

0

2

# Physics 2080; Chapter 29 Part B Notes Physics 2080

Marketplace > Clemson University > Physics 2 > Physics 2080 > Physics 2080 Chapter 29 Part B Notes
Amanda Biddlecome
Clemson
GPA 4.0

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These notes cover the end of chapter 29 and a few final tips from our review session for the test.
COURSE
General Physics 2
PROF.
Dr. Pope
TYPE
Class Notes
PAGES
2
WORDS
CONCEPTS
Physics
KARMA
25 ?

## Popular in Physics 2

This 2 page Class Notes was uploaded by Amanda Biddlecome on Tuesday April 12, 2016. The Class Notes belongs to Physics 2080 at Clemson University taught by Dr. Pope in Fall 2016. Since its upload, it has received 23 views. For similar materials see General Physics 2 in Physics 2 at Clemson University.

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Date Created: 04/12/16
Physics  2080   Chapter  29  Part  B     April  10,  2016   Amanda  Biddlecome     1)  Relativistic  Energy     -­‐if  things  gain  mass,  the  energy  increases     E=(m c )/√(1-0‐(v /c ))   2 2 *gives  total  energy   *m =re0ting  mass   *c=speed  of  light   *v=velocity     E =m c   2 0 0 *resting  mass  energy  when  velocity  is  0       -­‐Kinetic  Energy     K=E-­‐E 0       -­‐positron  and  electron  collide  and  annihilate  each  other       *they  have  the  same  mass  and  equal  but  opposite  charges       *emit  energy  in  the  form  of  electromagnetic  radiation     -­‐at  normal  speeds,  the  classic  kinetic  energy  and  relativistic  kinetic  energy     are  the  same     2)  General  Relativity     -­‐used  in  satellites,  medicine,  and  space  exploration     -­‐Principle  of  Equivalence       *all  experiments  done  in  a  uniform  gravitation  field  and  in  an           accelerated  frame  of  reference  give  identical  results       *light  shining  in  an  accelerated  elevator  bends  downward       *tells  us  that  light  should  bend  in  a  gravitational  field     -­‐we  can  see  the  Principle  of  Equivalence  during  a  solar  eclipse     -­‐black  hole=when  light  is  bent  so  much  that  it  can’t  leave  the  gravitational     field     R=2GM/c   2 *R=radius  of  a  black  hole       -­‐imagine  space  and  time  is  bent  to  visualize  gravitational  waves       *we  were  able  to  measure  this  this  year       *two  black  holes  circled  each  other  until  they  collided;  made  a  smaller       black  hole  and  the  extra  energy  was  given  off  as  gravitational  waves   Exam  Tips:     *virtual  images  are  always  negative   *one  wavelength  behind  is  constructive  and  creates  bright  fringes,  one  half  a   wavelength  behind  is  destructive  and  creates  dark  fringes   *λ=c/f   *length  contracts  along  the  direction  of  motion   *a  person  in  a  spaceship  traveling  towards  land  will  be  the  one  that  sees  the   contracted  length   *period  (seconds)=1/frequency

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