View source for Astronomy college course/Introduction to stellar measurements


===A few definitions===
* Luminosity: In astronomy, ''luminosity'' is total amount of energy emitted by a star or other astronomical object per unit time. In SI units this is expressed as joules per second or watts. I.e. The Sun has a total power output of 3.846×10<sup>26</sup> Watts (that's a lot of light bulbs!).  A more convenient unit of luminosity is this Sun itself: 1.00 solar luminosity, or <math>1\,L_\odot\approx3.85\times10^{26}\,W\,</math>.
* [[File:65Cyb-LB3-apmag.jpg|60px|thumb]][[w:Relative magnitude|Relative magnitude]]: a numerical measure of an astronomical object ''as seen from Earth''; a decrease of 1 unit represents an increase in the light received by a factor of 2.512. In other words, the larger the relative magnitude, the fainter the object appears to be.<ref>https://en.wiktionary.org/w/index.php?title=apparent_magnitude&oldid=23450540</ref>
* [[w:Absolute magnitude|Absolute magnitude]]: a numerical measure of an astronomical object as seen from a distance of 10 parsecs or 32.6 light years.  An object's relative and absolute magnitudes are equal if and only if teh object is 10 parsecs from Earth (neglecting [[w:Extinction (astronomy)|extinction]] effects). As with relative magnitude words, the larger the absolute magnitude, the less luminous the object actually is.<ref>https://en.wiktionary.org/w/index.php?title=absolute_magnitude&oldid=24168207</ref>
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*[[w:Stellar parallax|Stellar parallax]]: The change of angular position of a star as seen from Earth, due to the motion of the Earth around the Sun. The star's angular shift that occurs when the observer moves by AU ([[w:one astronomical unit|one astronomical unit]]) In 1989 the satellite [[Hipparcos]] was launched primarily for obtaining parallaxes and [[w:proper motion|proper motnios]] allowing measurements of stellar parallax for stars up to about 500  parsecs away, a little more than one percent of the diameter of the [[w:Milky Way Galaxy|Milky Way Galaxy]].<ref>https://en.wikipedia.org/w/index.php?title=Stellar_parallax&oldid=586855433</ref>
* Standard candle: an astronomical object that has a known luminosity.

[[File:Extragalactic distance ladder.JPG|thumb|left|300px|A perplexing array of standard candles.  The fainter and more common nearby candles are used to calibrate the ultra-Luminous and exotic objects that allow us to measure distances reaching billions of light years away.]]The figure to the left shows what Wikipedia calls the [[w:Cosmic distance ladder]].<ref>https://en.wikip
edia.org/w/index.php?title=Cosmic_distance_ladder&oldid=600781949</ref> The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.

==Equations==
===Angular size, size, and distance===
*<math>s=r\theta_\mathrm{rad}\approx r\frac{\theta_\mathrm{deg}}{57.3}\,</math> &nbsp; is the [[w:arclength|arclength]] of a portion of a circle of radius ''r'' described the angle ''θ''. The two forms allow  ''θ'' to be measured in either degrees or radians (2π rad = 360 deg). The lengths ''r'' and ''s'' must be measured in the same units. 

[http://physics.weber.edu/schroeder/ua/HandAngles.png Using your hand to measure angules]

===Stellar parallax===

{{#lst:Physics_equations/Equations|AstrParallax}}

===Newton's version of Kepler's third law===
Kepler (1571-1630) found a relation between period and average distance for all planets and comets around the Sun.  Newton (1643-1727) discovered "universal" laws  which not only explained Kepler's third law, but showed that the applied on earth, around other planets, as well as for stars and clusters of stars.  His addition of the "total mass" allows us to "weigh" (technically "mass" almost anything and everything in the universe.

{{#lst:Physics_equations/Equations|KeplerNewtonMassPeriodDistanceNorm}}

===Normalized units===
Kepler's third law is a relation between the period of a planet and an averaged distance (semi-major axis) from the Sun.  It takes on a simple form if the period is measured in years and the distance is measured in AU.  For Earth, we have:

:<math>a^3=P^2\rightarrow 1^3=1^2\;</math>

In contrast, if time is measured in seconds and distance in meters, then the Kepler's third law for Earth looks like this:

:<math>a^3=  \frac{M_\odot G}{4\pi^2}P^2\rightarrow (1.5\times 10^{11})^3=</math><math>
\frac{(1.99\times 10^{30})(6.67\times 10^{-11})}{4\pi^2}(3.16\times 10^{7})^2 </math>

In the previous section, the Kepler/Newton relation between mass, period and semi-major axis are most conveniently written using the following units:
* Time is measured in years
* Distance is measured in AU
* Mass is measured in solar masses.

In the next sections, we find it helpful to define:
* Power (L) is measured in units of the Sun's power output
* Temperature (T) is measured in units of the Sun's temperature.
* Radius (R) is measured in units of the Sun's radius.

To remind the reader that these [[w:Nondimensionalization|normalized]], a tilde shall be placed over the variables.  If a star's temperature is expressed as <math>\tilde T = 0.5</math> and its radius is <math>\tilde R = 100</math>, then its surface is half that of the Sun, and it is 100 times larger than the Sun.

===Two facts about how blackbodies "glow"===
A hot object gives off electromagnetic radiation.  We sometimes experience this as visible light given off by every hot objects, or as heat given off by a campfire.  While these phenomena have been observed for centuries, a mathematical understanding only emerged only by the first decade of the 20th century with the revolutionary idea that light was both a particle ('photon') and a wave.  The following formulas are strictly true only for a blackbody, but they are good approximations for stars, since most photons that strike a star get 'lost' in the star.  The color of a black body is closely related to it's temperature.  Here 'color' refers to the peak wavelength emitted by the star:

{{#lst:Physics_equations/Equations|AstrBlackbody}}

The [[w:Stefan-Boltzmann_constant|Stefan-Boltzmann constant]], σ, is a fundamental constant (like [[w:Gravitational constant|Newton's G]], [[w:Planck constant|Planck's h]], or even [[w:speed of light|Einstein's c]]).  
===Inverse square law===
[[w:Relative magnitude|Relative magnitude]] is a common measure of how bright an object appears to be from Earth.  Unfortunately this is a [[w:Logarithmic scale|Logarithmic scale]] that renders calculations somewhat advanced.  Instead we shall use intensity, normalized to units where power is measured in units of Solar luminosity:

{{#lst:Physics_equations/Equations|AstrInverseSquare}}


For example, I=1/4π for a star like the Sun situated one parsec away, provided intensity is measured as Solar luminosities per square parsec.  To see how much energy (or power) enters a telescope, it is necessary to calculate the area of the telescope in square parsecs.

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(Many are from [https://en.wiktionary.org/wiki/Wiktionary:Main_Page Wiktionary])
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[[Category:Intro astronomy college course]]
[[Category:Astronomy college course]]