Cheatography

# Intro to Astronomy Cheat Sheet (DRAFT) by bittbobitty

Exam Revision

This is a draft cheat sheet. It is a work in progress and is not finished yet.

### Keplar

 The Law of Ellipses The path of the planets around the sun is elliptical in shape, with the centre of the sun being located at one focus. The Law of Equal Areas An imaginary line drawn from the centre of the sun to the centre of the planet will sweep out equal areas in equal intervals of time. The Law of Harmonies The ratio of the squares of the periods of any two planets is equal to the ratio of the cubes of their average distances from the sun.

### Parallax

Parallax is the apparent displa­cement of an object because of a change in the observer's point of view.
Equation is d = 1/p where;
d = distance measured in parsecs
p = parallax angle measured in arcseconds

### Special Relativity

 Definition Mass and energy are the same physical entity and can be changed into each other. E = mc^2 The increased relati­vistic mass (m) of a body times the speed of light squared (c^2) is equal to the kinetic energy (E) of that body. The Sun The nuclear fusion reactions that transform hydrogen to helium are part of the reason that the sun shines. The energy released from the rest energy of hydrogen atoms that are fused to form helium.

### Star Luminosity and Distance

 The size of a star If two stars have the same effective temper­ature but differ in size then the larger star has a greater surface area and as it radiates the same amount of energy per unit surface area per second as the smaller star its total power output or luminosity will be greater. The distance to the star The closer the star the brighter it will appear. Luminosity The intrinsic brightness of a celestial object. Apparent Magnitude The magnitude of a celestial object as it is actually measured from the Earth. Absolute Magnitude The magnitude (brigh­tness) of a celestial object as it would be seen at a standard distance of 10 parsecs.

### HR Diagram

 1. The main sequence stretching from the upper left (hot, luminous stars) to the bottom right (cool, faint stars) dominates the HR diagram. It is here that stars spend about 90% of their lives burning hydrogen into helium in their cores. 2. Red giant and supergiant stars (lumin­osity classes I through III) occupy the region above the main sequence. They have low surface temper­atures and high lumino­sities which means they also have large radii. Stars enter this stage after they have exhausted the hydrogen fuel in their cores and have started to burn helium and other heavier elements. 3. White dwarf stars (lumin­osity class D) are the final evolut­ionary stage of low to interm­ediate mass stars, and are found in the bottom left of the HR diagram. These stars are very hot but have low lumino­sities due to their smaller size.

### EM Spectrum

Radio waves have the lowest frequency

### Solar Time

 Apparent Solar Time Observed from Earth. Based on the apparent motion of the actual sun. It is based on the apparent solar day, the interval between two successive returns of the sun to the local meridian. Mean Solar Time Is the hour angle of the sun plus twelve hours.

### Sun's Surface

 Sunspots are visible as dark patches on the sun's photos­phere, and correspond to concen­tra­tions of magnetic field where the convective transport of heat is inhibited from the solar interior to the surface. As a result, sunsports are slightly cooler than the surrou­nding photos­phere, and, so, they appear dark.

### Magnet­osphere

 Is the region around a planet dominated by the planet's magnetic field. Other planets in our solar system have magnet­osp­heres, but Earth has the strongest one of all the rocky planets. It shields the planet from solar and cosmic particle radiation, as well as erosion of the atmosphere by the solar wind - the constant flow of charged particles streaming off the sun.

### Basic Defini­tions

 Displa­cement or Distance (d) Change in position of an object. Measured in metres (m). Specified by difference in initial and final coordi­nates, d = xf - xi Velocity Distance travelled per unit time and the direction of motion. Measured in (m/s). Speed The magnitude of the velocity (no direction specified) v = d/t Accele­ration A change in velocity per unit time and the direction of that change. Measured in metres per second per second (m/s^2). a = (vf - vi)/t (for constant a). Mass A property of matter that determines how resistant an object is to changes in motion and how strong a gravit­ational force it exerts and experi­ences in the presence of another object. Measured in kg. Distance Equation d = vit + (1/2)at^2

### Newton's Laws

 Inertia The velocity of an object doesn't change unless you apply a force. Momentum p = mv. Impulse is the same as force. Equal and Opposite Reactions Force always comes in pairs. Equal in magnitude by opposite in direction.

### Waves

 Deinition A propag­ating distur­bance in a stable, extended medium. The properties of the medium determine the behaviour of the waves. The medium does not move. Waves carry energy and momentum. Reflection The incoming angle (incid­ence) equals the outgoing angle (refle­ction). Refraction When waves move between one medium and another and propagate at different speeds in the two media, the wave direction will bend. This is a direct conceq­uence of the different speeds. Doppler Effect Wavelength changes if source is moving Interf­erence Constr­uctive or destru­ctive Resonance Freque­ncies determined by structural properties and can be excited.

### Seismic Waves

 P WAVES S WAVES Primary Secondary Pressure (sound) Shear Longit­udinal Transverse Faster Slower Least damage Most damage Can travel through both solid and liquid Can travel through solid, not liquid