1Class 6Orbits and Tides Orbits Energy The different kinds of orbits Escape velocity Tides in the Earth-Moon systemI : Orbital energy The energy of the orbit is one of the most importantdefining quantities: consider a particle of mass m in anorbit about a (much larger) mass M. Then… Kinetic energy of particle is Gravitational potential energy of particle is Total energy is just the sum… Total energy remains unchanged (it is conserved) asparticle orbits… but it can trade between kinetic andpotential form.2All of these shapes are “conic sections”The total energy of the orbit determines the form… E<0 ⇒ elliptical orbit The maximum possible distance that the particle canget to corresponds to having all of the energy ingravitational potential energy… This is a bound orbit A special case if that of a circular orbit…F=ma for circular motionin a gravitational field3THE BLACK HOLE IN M106 Notes:4 E=0 ⇒ parabolic orbit Orbit has mathematical form of y=x2 Particle starts “at rest at infinity”, falls in, swings bycentral object and heads back out to “infinity at rest”. Orbit is marginally unbound Particularly simple relationship between speed andposition E>0 ⇒ hyperbolic orbit Orbit has mathematically form x2-y2=constant Unlike parabolic case, particle has non-zero velocityeven when it is far from the gravitating mass (i.e.“at infinity”) This is an unbound orbit5II : Escape velocity Another important use of the energy equationis calculation of “escape velocity” Definition : The escape velocity from a planet’ssurface is the speed that needs to be given to aparticle in order for it to reach “infinity” This is just the speed needed to put it on a parabolicorbit… Escape velocity is very important concept…6 Early ideas for black holes Laplace (1798) – “A luminous star, of the samedensity as the Earth, and whose diameter should betwo hundred and fifty times larger than that of theSun, would not, in consequence of its attraction,allow any of its rays to arrive at us; it is thereforepossible that the largest luminous bodies in theuniverse may, through this cause, be invisible.” Rev. John Mitchell had same idea 15 years earlier(1783)III : Tides in the Earth-Moonsystem Consider the gravitational force exerted by theMoon on various parts of the Earth…7 The point of the Earth closest to the Moon “feels” astronger gravitational force from the Moon than apoint on the opposite side of the Earth. These differential forces are known as tidal forces;they stretch the Earth along the line connecting it tothe Moon, and squeeze the Earth in theperpendicular direction The oceans respond to the stretching/squeezingmuch more than the solid Earth… gives rise to thefamiliar notion of tides8The Sun alsohas an effect But there’s a lot more to tides than justchanges in sea-level… The “tidal bulge” is slightly misaligned with the lineconnecting the center of the Earth and the Moon…the Earth’s rotation “drags” it slightly ahead.Figure from Robin Shelton’s webpagehttp://www.physast.uga.edu/~rls/1020/ch5/9 DISCUSSION : What are the consequences of