D1 Gravitational fields

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16 Terms

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D1.1 Newton’s law of gravitation

Gravitational force between 2 bodies outside a uniform field; earth-sun → The gravitational force between two point masses is to m1m2 and inversely to the square of their separation (r2)

F = GM(1)m2/r2 = force felt by either body.
G = Newtons Gravitational Constant: 6.67×10-11 Nkg-2m2
r = distance centre mass 1 mass 2

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D1.2 Gravitational Field Strength

Force due to gravity = weight
Gravitational field: region of space where test mass experiences force due to grav. attraction of another mass.
ALWAYS ATTRACTIVE!!!
grav field strength = force per unit mass experienced by test mass at that point → g = F/m2 = GM(1)/r2
M causes grav field, all bodies at same r2 receive same grav field stren

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D1.3 Uniform sphere → point mass

Uniform sphere; point mass → uniform distribution of mass (density)
→ field lines are uniform around sphere and thus around point mass

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D1.4 Field lines

Directed towards centre of mass. Size of field proportional to line density. Direction shows acceleration of acceleration of point mass put into the field.
Point mass: radially inwards: non uniform field; line density ∝ field
Earth’s surface (straight and faaar): par. lines spaced equ:uniform field

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D1.5 Grav Potential

V = W done per unit mass in bringing test mass from ∞ to defined point
J kg-1. ALWAYS negative: attractive force. at ∞, V = 0, so work must be done to reach infinity, and work is “released” when “falling” to defined point. As object moves away from “planet” - less increases.

Vg = - GM/r
r = distance centre of mass to point mass.
SCALAR
In uniform field: ΔV = g Δh

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D1.6 Grav Pot Energy

In non-uniform field (g depends on r)
GPE - energy objects possesses due to position in field
→ Work done in bringing mass from ∞ to point

Near earth surface: uniform field: Ep = mgΔh: work done to lift object
non unif. field: ΔGPE = W = mΔVg (m=of small object)
Change in ΔEp = W = GMm (1/r1 - 1/r2)
Ep = -GMm/r = -Fr (as we known, as work done = Fr)
Graph F - r : area = work done

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D1.7 Grav Pot gradient

g at a particular point = -(gradient of a V-r graph at that point)
g = - ΔVg/Δr (g = positive…)

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D1.8 Grav Equipotential surfaces

Equipotential lines: like wavefronts; perpendicular to field lines

All points on one line have same grav potential.

Dotted lines, no arrows

Uniform field = uniform ditance

No work is done when moving along an equipotential line/surface ( eg. earths surface)

ΔV = 0.

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D1.9 Keplers 1st law of planetary motion

SHAPE 1st law: orbit of a planet is an ellipse and sun is at one of the 2 foci (focus is at point where red distance is constant throughout ellipse.)

<p>SHAPE 1<sup>st</sup> law: orbit of a planet is an ellipse and sun is at one of the 2 foci (focus is at point where red distance is constant throughout ellipse.)</p>
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D1.10 Keplers 2nd law

MOTION 2nd law: all line segments joining sun to planet sweep equal area in equal time intervals.
Shows that planets move faster near sun and slower further away from it.

<p>MOTION 2nd law: all line segments joining sun to planet sweep equal area in equal time intervals.<br>Shows that planets move faster near sun and slower further away from it. </p>
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D1.11 Kepler’s 3rd law

3rd law: For planets/satelites in circular orbit about same body; Time period2 ∝ radius of orbit3

2 log T ∝ 3 log r

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D1.12 Time period and orbital radius relation

v = 2πr/T
v2 = (2πr/T)2 = GM/r (centripetal force)
T2 = (4π2r3)/GM

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D1.13 Escape speed

Minimum v alowin object to escape grav. field with no other E input

Same for all masses in same grav. field.
½ vesc2 = GM/r (Ek = energy/m needed to overcome grav potential energy up to infinity = -Ep)
vesc = √ (2GM/r)

Rockets launched from earth surface dont need to achieve escape v to reach orbit around earth; continuously fueled, not whole field is escaped, only to get to its orbit (centripetal force keeps it spinning)

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D1.14 Orbital speed

Most planets/satelites have near circular orbits; Fg → Fcentripetal
Both Fg & Fc are perp to direction of travel.
Fg = Fcirc
GMm/r2 = mv2/r
vorb = √ (GM/r) ——no matter mass of plan/sat, same vorb
r = centre of M to satellite.

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D1.15 Orbital Energy

ET = Ek + Ep
Ep = -2Ep
ET = -Ek = Ep/2

<p>E<sub>T</sub> = E<sub>k</sub> + E<sub>p</sub><br>E<sub>p</sub> = -2E<sub>p</sub><br>E<sub>T  </sub>= -E<sub>k</sub> = <sup>E</sup><sub><sup>p</sup></sub>/<sub>2</sub></p>
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D1.16 Drag in orbital motion

In low orbits (<600km), satelites may experience viscous drag (air

very small, but over time has signif. on height and speed of orbit

get closer to earth until hits it (radius decreases, v increases)
Ek → Q (friction air particles and surface of satellite.