Editing Tip of the red-giant branch (section)

==Method==
[[File:M5 colour magnitude diagram.png|thumb|left|upright=1.2|[[Hertzsprung–Russell diagram]] for [[globular cluster]] [[Messier 5|M5]]. The red-giant branch runs from the thin horizontal [[subgiant|subgiant branch]] to the top right, with a number of the more luminous RGB stars marked in red.]]
The [[Hertzsprung–Russell diagram]] (HR diagram) is a plot of stellar luminosity versus surface temperature for a population of stars. During the core hydrogen burning phase of a Sun-like star's lifetime, it will appear on the HR diagram at a position along a diagonal band called the [[main sequence]]. When the hydrogen at the core is exhausted, energy will continue to be generated by hydrogen fusion in a shell around the core. The center of the star will accumulate the helium "ash" from this fusion and the star will migrate along an evolutionary branch of the HR diagram that leads toward the upper right. That is, the surface temperature will decrease and the total energy output (luminosity) of the star will increase as the surface area increases.<ref name="harpaz">{{cite book | first=Amos | last=Harpaz | date=1994 | title=Stellar evolution | series=Peters Series | pages=103–110 | publisher=A K Peters, Ltd. | isbn=978-1-56881-012-6}}</ref>

At a certain point, the helium at the core of the star will reach a pressure and temperature where it can begin to undergo nuclear fusion through the [[triple-alpha process]]. For a star with less than 1.8 times the [[solar mass|mass of the Sun]], this will occur in a process called the [[helium flash]]. The [[evolutionary track]] of the star will then carry it toward the left of the HR diagram as the surface temperature increases under the new equilibrium. The result is a sharp discontinuity in the evolutionary track of the star on the HR diagram.<ref name="harpaz" /> This discontinuity is called the tip of the red-giant branch.

When distant stars at the TRGB are measured in the [[I band (infrared)|I-band]] (in the infrared), their luminosity is somewhat insensitive to their composition of elements heavier than helium ([[metallicity]]) or their mass; they are a [[standard candle]] with an I-band [[absolute magnitude]] of –4.0±0.1.<ref>{{cite conference | title= The Tip of the Red Giant Branch as a Population II Distance Indicator | author=Sakai, S | bibcode=1999IAUS..183...48S | conference= Proceedings of the 183rd symposium of the International Astronomical Union | editor= Katsuhiko Sato | date=1999 | publisher= Dordrecht, Boston: Kluwer Academic}}</ref> This makes the technique especially useful as a distance indicator. The TRGB indicator uses stars in the old stellar populations ([[Population II]]).<ref name="Ferrareseetal2000">{{cite journal |display-authors=6 |last1=Ferrarese |first1=Laura |last2=Ford |first2=Holland C. |last3=Huchra |first3=John |last4=Kennicutt, Jr. |first4=Robert C. |last5=Mould |first5=Jeremy R. |last6=Sakai |first6=Shoko |last7=Freedman |first7=Wendy L. |last8=Stetson |first8=Peter B. |last9=Madore |first9=Barry F. |last10=Gibson |first10=Brad K. |last11=Graham |first11=John A. |last12=Hughes |first12=Shaun M. |last13=Illingworth |first13=Garth D. |last14=Kelson |first14=Daniel D. |last15=Macri |first15=Lucas |last16=Sebo |first16=Kim |last17=Silbermann |first17=N. A. |title=A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations |journal=The Astrophysical Journal Supplement Series |year=2000 |volume=128 |issue=2 |pages=431–459 |bibcode=2000ApJS..128..431F |doi=10.1086/313391 |type=abstract |arxiv=astro-ph/9910501 |s2cid=121612286}}</ref>