<h3>Stellar Parallax</h3>
<p>Stellar parallax uses differences in perspective to determine the distance from an object. When the earth goes around the sun, our perspective of the star, galaxy etc. changes and so the angle from us to the object changes. Because we know how the earth moves around the sun, we know the distance between the points that we take the measurements. From this we can use the <a href="http://en.wikipedia.org/wiki/Law_of_sines" rel="noreferrer">Sine Rule</a> to determine the distance from the object.</p>
<p>For Example, if the distance between the two points of measurement were 2 units, and the two inside angles (<em>A</em> and <em>B</em>) were (<em>A</em>)80° and (<em>B</em>)75° (and therefore the other angle (<em>C</em>) is 25°) we can say that:</p>
<p><span class="math-container">$a = \frac{2\sin80}{\sin25}\ $</span></p>
<p>where &quot;<em>a</em>&quot; is the opposite side to angle &quot;<em>A</em>&quot;. This means that the distance between the object and the <em><strong>second</strong></em> (<em>B</em>) point of measurement is approximately 4.66 units.
<a href="https://i.sstatic.net/5ObPo.png" rel="noreferrer">Diagram here</a>.</p>
<hr />
<h3>Standard Candles</h3>
<blockquote> A standard candle is an astronomical object that has a known absolute magnitude. (<a href="http://astronomy.swin.edu.au/cosmos/S/Standard+Candle" rel="noreferrer">source</a>) </blockquote> 
<p>By using the known absolute and the measured <em>apparent magnitude</em> (what is seen by instruments etc.) it is possible to determine the distance of the object by using the formula:</p>
<blockquote>
<p>m-M = 5 log d – 5<br />
where <em>m</em> is the apparent magnitude of the object, <em>M</em> is the absolute magnitude of the object, and <em>d</em> is the distance to the object in parsecs.(<a href="http://astronomy.swin.edu.au/cosmos/S/Standard+Candle" rel="noreferrer">same source</a>)</p>
</blockquote>
<p>One of the most widely used examples of these standard candles is the supernovae type Ia, which was used to discover that the universe is accelerating in its expansion. This led to the awarding of the 2011 Nobel Prize in Physics to <a href="http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/perlmutter-facts.html" rel="noreferrer">Saul Perlmutter</a>, <a href="http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/schmidt-facts.html" rel="noreferrer">Brian Schmidt</a> , and <a href="http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/riess-facts.html" rel="noreferrer">Adam Riess</a>.</p>
<p>Additionally, <a href="http://en.wikipedia.org/wiki/RR_Lyrae_variable" rel="noreferrer">RR Lyrae</a> are another form of standard candle used to measure galactic distances (SN Ia are much more luminous and therefore can be used to much higher distances). RR Lyrae are a type of variable star with a relationship between pulsation period and absolute magnitude, which is what makes them good for use as standard candles.</p>
<p>Other information <a href="http://astronomy.swin.edu.au/cosmos/S/Standard+Candle" rel="noreferrer">here</a>.</p>
<hr />
<h3>Redshift</h3>
<p>Redshift is the effect where light from an object is &quot;stretched&quot; out so that the wavelength is moved towards the &quot;red&quot; end of the spectrum. Distances are calculated by using Hubble's Law, but I'll let others explain it: <a href="http://www.astro.cornell.edu/academics/courses/astro201/hubbles_law.htm" rel="noreferrer">here</a>, <a href="http://hyperphysics.phy-astr.gsu.edu/hbase/astro/hubble.html" rel="noreferrer">here</a> and <a href="http://csep10.phys.utk.edu/astr162/lect/cosmology/hubble_constant.html" rel="noreferrer">here</a>.</p>

CC BY-SA 3.0
2014-07-26T12:49:07.713Z
I stumbled upon this recent idea to use gamma ray bursts as a distance measure (by Z Cano in Iceland). I think you'll have to keep adding things to your list there, the question of distances in the universe is under continuous study ;-) http://astrobites.org/2014/07/14/can-gamma-ray-bursts-be-used-as-standard-candles/
LocalFluff
CC BY-SA 3.0
2013-10-10T11:54:38.123Z
@myself To do list: Add angular diameter distances, luminosity distance, and lyman alpha forest to this post (just to name a few others).
astromax
CC BY-SA 3.0
2013-09-25T08:58:13.880Z
2014-07-26T00:45:49.640Z
2020-06-17T09:47:40.653Z
damned truths
<p>Distances in our universe can be calculated in several ways: </p>

<ul>
<li>Stellar Parallax</li>
<li>Standard Candles</li>
<li>Redshift</li>
</ul>

<p>How are these methods linked, and how they are actually used to calculate   distances are measured in the Solar System, in the Galaxy, and in the Universe?</p>

CC BY-SA 3.0
2013-09-25T04:39:27.530Z
[Cosmic Distance Ladder](http://en.wikipedia.org/wiki/Cosmic_distance_ladder)
Guillochon
<distances><parallax><redshift>
How distances are measured in the Solar System, in the Galaxy, and in the Universe?
leonard vertighel
# How distances are measured in the Solar System, in the Galaxy, and in the Universe?

(Asked by: username_0 on 2013-09-25)

Distances in our universe can be calculated in several ways:

* Stellar Parallax
* Standard Candles
* Redshift

How are these methods linked, and how they are actually used to calculate distances are measured in the Solar System, in the Galaxy, and in the Universe?

**Tags:** distances, parallax, redshift

> **Comments:**
> **username_1**: [Cosmic Distance Ladder](http://en.wikipedia.org/wiki/Cosmic_distance_ladder)  

---

## 1 answers

### Answer by username_2 on 2013-09-25. Score: 13

### Stellar Parallax

Stellar parallax uses differences in perspective to determine the distance from an object. When the earth goes around the sun, our perspective of the star, galaxy etc. changes and so the angle from us to the object changes. Because we know how the earth moves around the sun, we know the distance between the points that we take the measurements. From this we can use the [Sine Rule](http://en.wikipedia.org/wiki/Law_of_sines) to determine the distance from the object.

For Example, if the distance between the two points of measurement were 2 units, and the two inside angles (*A* and *B*) were (*A*)80° and (*B*)75° (and therefore the other angle (*C*) is 25°) we can say that:

$a = \frac{2\sin80}{\sin25}\ $

where "*a*" is the opposite side to angle "*A*". This means that the distance between the object and the ***second*** (*B*) point of measurement is approximately 4.66 units.
[Diagram here](https://i.sstatic.net/5ObPo.png).

---

### Standard Candles

> A standard candle is an astronomical object that has a known absolute magnitude. ([source](http://astronomy.swin.edu.au/cosmos/S/Standard+Candle))

By using the known absolute and the measured *apparent magnitude* (what is seen by instruments etc.) it is possible to determine the distance of the object by using the formula:

> m-M = 5 log d – 5  
> where *m* is the apparent magnitude of the object, *M* is the absolute magnitude of the object, and *d* is the distance to the object in parsecs.([same source](http://astronomy.swin.edu.au/cosmos/S/Standard+Candle))

One of the most widely used examples of these standard candles is the supernovae type Ia, which was used to discover that the universe is accelerating in its expansion. This led to the awarding of the 2011 Nobel Prize in Physics to [Saul Perlmutter](http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/perlmutter-facts.html), [Brian Schmidt](http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/schmidt-facts.html) , and [Adam Riess](http://www.nobelprize.org/nobel_prizes/physics/laureates/2011/riess-facts.html).

Additionally, [RR Lyrae](http://en.wikipedia.org/wiki/RR_Lyrae_variable) are another form of standard candle used to measure galactic distances (SN Ia are much more luminous and therefore can be used to much higher distances). RR Lyrae are a type of variable star with a relationship between pulsation period and absolute magnitude, which is what makes them good for use as standard candles.

Other information [here](http://astronomy.swin.edu.au/cosmos/S/Standard+Candle).

---

### Redshift

Redshift is the effect where light from an object is "stretched" out so that the wavelength is moved towards the "red" end of the spectrum. Distances are calculated by using Hubble's Law, but I'll let others explain it: [here](http://www.astro.cornell.edu/academics/courses/astro201/hubbles_law.htm), [here](http://hyperphysics.phy-astr.gsu.edu/hbase/astro/hubble.html) and [here](http://csep10.phys.utk.edu/astr162/lect/cosmology/hubble_constant.html).

> **Comments:**
> **username_4**: @myself To do list: Add angular diameter distances, luminosity distance, and lyman alpha forest to this post (just to name a few others).  
> **username_3**: I stumbled upon this recent idea to use gamma ray bursts as a distance measure (by Z Cano in Iceland). I think you'll have to keep adding things to your list there, the question of distances in the universe is under continuous study ;-) http://astrobites.org/2014/07/14/can-gamma-ray-bursts-be-used-as-standard-candles/  

---

