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Hertzsprung–Russell diagram

January 01, 1970

"H-R" redirects here. For other, see HR (disambiguation).

The Hertzsprung–Russell diagram (abbreviated as H–R diagram, HR diagram or HRD) is a scatter plot of stars showing the relationship between the stars' absolute magnitudes or luminosities and their stellar classifications or effective temperatures. The diagram was created independently in 1911 by Ejnar Hertzsprung and by Henry Norris Russell in 1913, and represented a major step towards an understanding of stellar evolution.

An observational Hertzsprung–Russell diagram with 22,000 stars plotted from the Hipparcos Catalogue and 1,000 from the Gliese Catalogue of nearby stars. Stars tend to fall only into certain regions of the diagram. The most prominent is the diagonal, going from the upper-left (hot and bright) to the lower-right (cooler and less bright), called the main sequence. In the lower-left is where white dwarfs are found, and above the main sequence are the subgiants, giants and supergiants. The Sun is found on the main sequence at luminosity 1 (absolute magnitude 4.8) and B−V color index 0.66 (temperature 5780 K, spectral type G2V).

Historical background edit

In the nineteenth century large-scale photographic spectroscopic surveys of stars were performed at Harvard College Observatory, producing spectral classifications for tens of thousands of stars, culminating ultimately in the Henry Draper Catalogue. In one segment of this work Antonia Maury included divisions of the stars by the width of their spectral lines.[1] Hertzsprung noted that stars described with narrow lines tended to have smaller proper motions than the others of the same spectral classification. He took this as an indication of greater luminosity for the narrow-line stars, and computed secular parallaxes for several groups of these, allowing him to estimate their absolute magnitude.[2]

In 1910 Hans Oswald Rosenberg published a diagram plotting the apparent magnitude of stars in the Pleiades cluster against the strengths of the calcium K line and two hydrogen Balmer lines.[3] These spectral lines serve as a proxy for the temperature of the star, an early form of spectral classification. The apparent magnitude of stars in the same cluster is equivalent to their absolute magnitude and so this early diagram was effectively a plot of luminosity against temperature. The same type of diagram is still used today as a means of showing the stars in clusters without having to initially know their distance and luminosity.[4] Hertzsprung had already been working with this type of diagram, but his first publications showing it were not until 1911. This was also the form of the diagram using apparent magnitudes of a cluster of stars all at the same distance.[5]

Russell's early (1913) versions of the diagram included Maury's giant stars identified by Hertzsprung, those nearby stars with parallaxes measured at the time, stars from the Hyades (a nearby open cluster), and several moving groups, for which the moving cluster method could be used to derive distances and thereby obtain absolute magnitudes for those stars.[6]

Forms of diagram edit

There are several forms of the Hertzsprung–Russell diagram, and the nomenclature is not very well defined. All forms share the same general layout: stars of greater luminosity are toward the top of the diagram, and stars with higher surface temperature are toward the left side of the diagram.

The original diagram displayed the spectral type of stars on the horizontal axis and the absolute visual magnitude on the vertical axis. The spectral type is not a numerical quantity, but the sequence of spectral types is a monotonic series that reflects the stellar surface temperature. Modern observational versions of the chart replace spectral type by a color index (in diagrams made in the middle of the 20th Century, most often the B-V color) of the stars. This type of diagram is what is often called an observational Hertzsprung–Russell diagram, or specifically a color–magnitude diagram (CMD), and it is often used by observers.[7] In cases where the stars are known to be at identical distances such as within a star cluster, a color–magnitude diagram is often used to describe the stars of the cluster with a plot in which the vertical axis is the apparent magnitude of the stars. For cluster members, by assumption there is a single additive constant difference between their apparent and absolute magnitudes, called the distance modulus, for all of that cluster of stars. Early studies of nearby open clusters (like the Hyades and Pleiades) by Hertzsprung and Rosenberg produced the first CMDs, a few years before Russell's influential synthesis of the diagram collecting data for all stars for which absolute magnitudes could be determined.[3][5]

Another form of the diagram plots the effective surface temperature of the star on one axis and the luminosity of the star on the other, almost invariably in a log-log plot. Theoretical calculations of stellar structure and the evolution of stars produce plots that match those from observations. This type of diagram could be called temperature-luminosity diagram, but this term is hardly ever used; when the distinction is made, this form is called the theoretical Hertzsprung–Russell diagram instead. A peculiar characteristic of this form of the H–R diagram is that the temperatures are plotted from high temperature to low temperature, which aids in comparing this form of the H–R diagram with the observational form.

Although the two types of diagrams are similar, astronomers make a sharp distinction between the two. The reason for this distinction is that the exact transformation from one to the other is not trivial. To go between effective temperature and color requires a color–temperature relation, and constructing that is difficult; it is known to be a function of stellar composition and can be affected by other factors like stellar rotation. When converting luminosity or absolute bolometric magnitude to apparent or absolute visual magnitude, one requires a bolometric correction, which may or may not come from the same source as the color–temperature relation. One also needs to know the distance to the observed objects (i.e., the distance modulus) and the effects of interstellar obscuration, both in the color (reddening) and in the apparent magnitude (where the effect is called "extinction"). Color distortion (including reddening) and extinction (obscuration) are also apparent in stars having significant circumstellar dust. The ideal of direct comparison of theoretical predictions of stellar evolution to observations thus has additional uncertainties incurred in the conversions between theoretical quantities and observations.

Interpretation edit

 
An HR diagram with the instability strip and its components highlighted

Most of the stars occupy the region in the diagram along the line called the main sequence. During the stage of their lives in which stars are found on the main sequence line, they are fusing hydrogen in their cores. The next concentration of stars is on the horizontal branch (helium fusion in the core and hydrogen burning in a shell surrounding the core). Another prominent feature is the Hertzsprung gap located in the region between A5 and G0 spectral type and between +1 and −3 absolute magnitudes (i.e., between the top of the main sequence and the giants in the horizontal branch). RR Lyrae variable stars can be found in the left of this gap on a section of the diagram called the instability strip. Cepheid variables also fall on the instability strip, at higher luminosities.

The H-R diagram can be used by scientists to roughly measure how far away a star cluster or galaxy is from Earth. This can be done by comparing the apparent magnitudes of the stars in the cluster to the absolute magnitudes of stars with known distances (or of model stars). The observed group is then shifted in the vertical direction, until the two main sequences overlap. The difference in magnitude that was bridged in order to match the two groups is called the distance modulus and is a direct measure for the distance (ignoring extinction). This technique is known as main sequence fitting and is a type of spectroscopic parallax. Not only the turn-off in the main sequence can be used, but also the tip of the red giant branch stars.[8][9]

The diagram seen by ESA's Gaia mission edit

 
Hertzsprung-Russell diagram showing only white dwarfs with data from ESA's Gaia mission
 
Part of the diagram from ESA's Gaia. The dark line likely represents the transition from partly convective to fully convective red dwarfs

ESA's Gaia mission showed several features in the diagram that were either not known or that were suspected to exist. It found a gap in the main sequence that appears for M-dwarfs and that is explained with the transition from a partly convective core to a fully convective core.[10][11] For white dwarfs the diagram shows several features. Two main concentrations appear in this diagram following the cooling sequence of white dwarfs that are explained with the atmospheric composition of white dwarfs, especially hydrogen versus helium dominated atmospheres of white dwarfs.[12] A third concentration is explained with core crystallization of the white dwarfs interior. This releases energy and delays the cooling of white dwarfs.[13][14]

Role in the development of stellar physics edit

See also: Stellar nucleosynthesis
 
HR diagrams for two open clusters, M67 and NGC 188, showing the main-sequence turn-off at different ages

Contemplation of the diagram led astronomers to speculate that it might demonstrate stellar evolution, the main suggestion being that stars collapsed from red giants to dwarf stars, then moving down along the line of the main sequence in the course of their lifetimes. Stars were thought therefore to radiate energy by converting gravitational energy into radiation through the Kelvin–Helmholtz mechanism. This mechanism resulted in an age for the Sun of only tens of millions of years, creating a conflict over the age of the Solar System between astronomers, and biologists and geologists who had evidence that the Earth was far older than that. This conflict was only resolved in the 1930s when nuclear fusion was identified as the source of stellar energy.

Following Russell's presentation of the diagram to a meeting of the Royal Astronomical Society in 1912, Arthur Eddington was inspired to use it as a basis for developing ideas on stellar physics. In 1926, in his book The Internal Constitution of the Stars he explained the physics of how stars fit on the diagram.[15] The paper anticipated the later discovery of nuclear fusion and correctly proposed that the star's source of power was the combination of hydrogen into helium, liberating enormous energy. This was a particularly remarkable intuitive leap, since at that time the source of a star's energy was still unknown, thermonuclear energy had not been proven to exist, and even that stars are largely composed of hydrogen (see metallicity), had not yet been discovered. Eddington managed to sidestep this problem by concentrating on the thermodynamics of radiative transport of energy in stellar interiors.[16] Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives. In the 1930s and 1940s, with an understanding of hydrogen fusion, came an evidence-backed theory of evolution to red giants following which were speculated cases of explosion and implosion of the remnants to white dwarfs. The term supernova nucleosynthesis is used to describe the creation of elements during the evolution and explosion of a pre-supernova star, a concept put forth by Fred Hoyle in 1954.[17] The pure mathematical quantum mechanics and classical mechanical models of stellar processes enable the Hertzsprung–Russell diagram to be annotated with known conventional paths known as stellar sequences—there continue to be added rarer and more anomalous examples as more stars are analysed and mathematical models considered.

See also edit

References edit

  1. ^ A.C. Maury; E.C. Pickering (1897). "Spectra of bright stars photographed with the 11-inch Draper Telescope as part of the Henry Draper Memorial". Annals of Harvard College Observatory. 28: 1–128. Bibcode:1897AnHar..28....1M.
  2. ^ Hertzprung, Ejnar (1908). "Über die Sterne der Unterabteilung c und ac nach der Spektralklassifikation von Antonia C. Maury". Astronomische Nachrichten. 179 (24): 373–380. Bibcode:1909AN....179..373H. doi:10.1002/asna.19081792402.
  3. ^ a b Rosenberg, Hans (1910). "Über den Zusammenhang von Helligkeit und Spektraltypus in den Plejaden". Astronomische Nachrichten. 186 (5): 71–78. Bibcode:1910AN....186...71R. doi:10.1002/asna.19101860503.
  4. ^ Vandenberg, D. A.; Brogaard, K.; Leaman, R.; Casagrande, L. (2013). "The Ages of 95 Globular Clusters as Determined Using an Improved   Method Along with Color-Magnitude Diagram Constraints, and Their Implications for Broader Issues". The Astrophysical Journal. 775 (2): 134. arXiv:1308.2257. Bibcode:2013ApJ...775..134V. doi:10.1088/0004-637X/775/2/134. S2CID 117065283.
  5. ^ a b Hertzsprung, E., 1911, Uber die Verwendung Photographischer Effektiver Wellenlaengen zur Bestimmung von Farbenaequivalenten, Publikationen des Astrophysikalischen Observatoriums zu Potsdam, 22. Bd., 1. Stuck = Nr.63
    Hertzsprung, E. (1911). "On the Use of Photographic Effective Wavelengths for the Determination of Color Equivalents". Publications of the Astrophysical Observatory in Potsdam. 1. 22 (63).
  6. ^ Russell, Henry Norris (1914). "Relations Between the Spectra and Other Characteristics of the Stars". Popular Astronomy. 22: 275–294. Bibcode:1914PA.....22..275R.
  7. ^ Palma, Christopher (2016). "The Hertzsprung-Russell Diagram". ASTRO 801: Planets, Stars, Galaxies, and the Universe. John A. Dutton e-Education Institute: College of Earth and Mineral Sciences: The Pennsylvania State University. Retrieved 2017-01-29. The quantities that are easiest to measure... are color and magnitude, so most observers ... refer to the diagram as a 'Color–Magnitude diagram' or 'CMD' rather than an HR diagram.
  8. ^ Da Costa, G. S.; Armandroff, T. E. (July 1990). "Standard globular cluster giant branches in the (MI,(V–I)O) plane". Astronomical Journal. 100: 162–181. Bibcode:1990AJ....100..162D. doi:10.1086/115500. ISSN 0004-6256.
  9. ^ Müller, Oliver; Rejkuba, Marina; Jerjen, Helmut (July 2018). "Tip of the Red Giant Branch Distances to the Dwarf Galaxies Dw1335-29 and Dw1340-30 in the Centaurus Group". Astronomy & Astrophysics. 615. A96. arXiv:1803.02406. Bibcode:2018A&A...615A..96M. doi:10.1051/0004-6361/201732455. S2CID 67754889.
  10. ^ "Mind the Gap: Gaia Mission Reveals the Insides of Stars". Sky & Telescope. 2018-08-06. Retrieved 2020-02-19.
  11. ^ Jao, Wei-Chun; Henry, Todd J.; Gies, Douglas R.; Hambly, Nigel C. (July 2018). "A Gap in the Lower Main Sequence Revealed by Gaia Data Release 2". Astrophysical Journal Letters. 861 (1): L11. arXiv:1806.07792. Bibcode:2018ApJ...861L..11J. doi:10.3847/2041-8213/aacdf6. ISSN 0004-637X. S2CID 119331483.
  12. ^ Collaboration, Gaia; Babusiaux, C.; van Leeuwen, F.; Barstow, M. A.; Jordi, C.; Vallenari, A.; Bossini, D.; Bressan, A.; Cantat-Gaudin, T.; van Leeuwen, M.; Brown, A. G. A. (August 2018). "Gaia Data Release 2. Observational Hertzsprung-Russell diagrams". Astronomy & Astrophysics. 616: A10. arXiv:1804.09378. Bibcode:2018A&A...616A..10G. doi:10.1051/0004-6361/201832843. ISSN 0004-6361.
  13. ^ "ESA Science & Technology - Gaia reveals how Sun-like stars turn solid after their demise". sci.esa.int. Retrieved 2020-02-19.
  14. ^ Tremblay, Pier-Emmanuel; Fontaine, Gilles; Fusillo, Nicola Pietro Gentile; Dunlap, Bart H.; Gänsicke, Boris T.; Hollands, Mark A.; Hermes, J. J.; Marsh, Thomas R.; Cukanovaite, Elena; Cunningham, Tim (January 2019). "Core crystallization and pile-up in the cooling sequence of evolving white dwarfs". Nature. 565 (7738): 202–205. arXiv:1908.00370. Bibcode:2019Natur.565..202T. doi:10.1038/s41586-018-0791-x. ISSN 0028-0836. PMID 30626942. S2CID 58004893.
  15. ^ Eddington, A. S. (Oct 1920). "The Internal Constitution of the Stars". The Scientific Monthly. 11 (4): 297–303. Bibcode:1920SciMo..11..297E. doi:10.1126/science.52.1341.233. JSTOR 6491. PMID 17747682.
  16. ^ Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society. 77: 16–35. Bibcode:1916MNRAS..77...16E. doi:10.1093/mnras/77.1.16.
  17. ^ Hoyle, F. (1954). "On Nuclear Reactions Occurring in Very Hot Stars. I. the Synthesis of Elements from Carbon to Nickel". Astrophysical Journal Supplement. 1: 121. Bibcode:1954ApJS....1..121H. doi:10.1086/190005.

Bibliography edit

  • Casagrande, L.; Portinari, L.; Flynn, C. (November 2006). "Accurate fundamental parameters for lower main-sequence stars". MNRAS. 373 (1): 13–44. arXiv:astro-ph/0608504. Bibcode:2006MNRAS.373...13C. doi:10.1111/j.1365-2966.2006.10999.x. S2CID 16400466.
  • Porter, Roy (2003). The Cambridge History of Science. Cambridge, UK: Cambridge University Press. p. 518. ISBN 978-0-521-57243-9.
  • Sekiguchi, Maki; Fukugita, Masataka (August 2000). "A Study of the B-V Color-Temperature Relation". The Astronomical Journal. 120 (2): 1072–1084. arXiv:astro-ph/9904299. Bibcode:2000AJ....120.1072S. doi:10.1086/301490. S2CID 14679334. Retrieved 2008-09-14.
  • Smith, Robert (1995). Observational Astrophysics. Cambridge, UK: Cambridge University Press. p. 236. ISBN 978-0-521-27834-8.

External links edit

 
Wikimedia Commons has media related to Hertzsprung–Russell diagram.
  • Omega Cen H-R animation of a Hertzsprung–Russell diagram created from real Hubble data
  • JavaHRD an interactive Hertzsprung–Russell diagram as a Java applet
  • BaSTI a Bag of Stellar Tracks and Isochrones, simulations with FRANEC code by Teramo Astronomical Observatory
  • Leos Ondra: The first Hertzsprung-Russell diagram
  • Who first published a Hertzsprung-Russell diagram? Hertzsprung or Russell? Answer: neither! 2021-05-15 at the Wayback Machine

January 01, 1970
hertzsprung, russell, diagram, redirects, here, other, disambiguation, abbreviated, diagram, diagram, scatter, plot, stars, showing, relationship, between, stars, absolute, magnitudes, luminosities, their, stellar, classifications, effective, temperatures, dia. H R redirects here For other see HR disambiguation The Hertzsprung Russell diagram abbreviated as H R diagram HR diagram or HRD is a scatter plot of stars showing the relationship between the stars absolute magnitudes or luminosities and their stellar classifications or effective temperatures The diagram was created independently in 1911 by Ejnar Hertzsprung and by Henry Norris Russell in 1913 and represented a major step towards an understanding of stellar evolution An observational Hertzsprung Russell diagram with 22 000 stars plotted from the Hipparcos Catalogue and 1 000 from the Gliese Catalogue of nearby stars Stars tend to fall only into certain regions of the diagram The most prominent is the diagonal going from the upper left hot and bright to the lower right cooler and less bright called the main sequence In the lower left is where white dwarfs are found and above the main sequence are the subgiants giants and supergiants The Sun is found on the main sequence at luminosity 1 absolute magnitude 4 8 and B V color index 0 66 temperature 5780 K spectral type G2V Contents 1 Historical background 2 Forms of diagram 3 Interpretation 3 1 The diagram seen by ESA s Gaia mission 4 Role in the development of stellar physics 5 See also 6 References 6 1 Bibliography 7 External linksHistorical background editIn the nineteenth century large scale photographic spectroscopic surveys of stars were performed at Harvard College Observatory producing spectral classifications for tens of thousands of stars culminating ultimately in the Henry Draper Catalogue In one segment of this work Antonia Maury included divisions of the stars by the width of their spectral lines 1 Hertzsprung noted that stars described with narrow lines tended to have smaller proper motions than the others of the same spectral classification He took this as an indication of greater luminosity for the narrow line stars and computed secular parallaxes for several groups of these allowing him to estimate their absolute magnitude 2 In 1910 Hans Oswald Rosenberg published a diagram plotting the apparent magnitude of stars in the Pleiades cluster against the strengths of the calcium K line and two hydrogen Balmer lines 3 These spectral lines serve as a proxy for the temperature of the star an early form of spectral classification The apparent magnitude of stars in the same cluster is equivalent to their absolute magnitude and so this early diagram was effectively a plot of luminosity against temperature The same type of diagram is still used today as a means of showing the stars in clusters without having to initially know their distance and luminosity 4 Hertzsprung had already been working with this type of diagram but his first publications showing it were not until 1911 This was also the form of the diagram using apparent magnitudes of a cluster of stars all at the same distance 5 Russell s early 1913 versions of the diagram included Maury s giant stars identified by Hertzsprung those nearby stars with parallaxes measured at the time stars from the Hyades a nearby open cluster and several moving groups for which the moving cluster method could be used to derive distances and thereby obtain absolute magnitudes for those stars 6 Forms of diagram editThere are several forms of the Hertzsprung Russell diagram and the nomenclature is not very well defined All forms share the same general layout stars of greater luminosity are toward the top of the diagram and stars with higher surface temperature are toward the left side of the diagram The original diagram displayed the spectral type of stars on the horizontal axis and the absolute visual magnitude on the vertical axis The spectral type is not a numerical quantity but the sequence of spectral types is a monotonic series that reflects the stellar surface temperature Modern observational versions of the chart replace spectral type by a color index in diagrams made in the middle of the 20th Century most often the B V color of the stars This type of diagram is what is often called an observational Hertzsprung Russell diagram or specifically a color magnitude diagram CMD and it is often used by observers 7 In cases where the stars are known to be at identical distances such as within a star cluster a color magnitude diagram is often used to describe the stars of the cluster with a plot in which the vertical axis is the apparent magnitude of the stars For cluster members by assumption there is a single additive constant difference between their apparent and absolute magnitudes called the distance modulus for all of that cluster of stars Early studies of nearby open clusters like the Hyades and Pleiades by Hertzsprung and Rosenberg produced the first CMDs a few years before Russell s influential synthesis of the diagram collecting data for all stars for which absolute magnitudes could be determined 3 5 Another form of the diagram plots the effective surface temperature of the star on one axis and the luminosity of the star on the other almost invariably in a log log plot Theoretical calculations of stellar structure and the evolution of stars produce plots that match those from observations This type of diagram could be called temperature luminosity diagram but this term is hardly ever used when the distinction is made this form is called the theoretical Hertzsprung Russell diagram instead A peculiar characteristic of this form of the H R diagram is that the temperatures are plotted from high temperature to low temperature which aids in comparing this form of the H R diagram with the observational form Although the two types of diagrams are similar astronomers make a sharp distinction between the two The reason for this distinction is that the exact transformation from one to the other is not trivial To go between effective temperature and color requires a color temperature relation and constructing that is difficult it is known to be a function of stellar composition and can be affected by other factors like stellar rotation When converting luminosity or absolute bolometric magnitude to apparent or absolute visual magnitude one requires a bolometric correction which may or may not come from the same source as the color temperature relation One also needs to know the distance to the observed objects i e the distance modulus and the effects of interstellar obscuration both in the color reddening and in the apparent magnitude where the effect is called extinction Color distortion including reddening and extinction obscuration are also apparent in stars having significant circumstellar dust The ideal of direct comparison of theoretical predictions of stellar evolution to observations thus has additional uncertainties incurred in the conversions between theoretical quantities and observations Interpretation edit nbsp An HR diagram with the instability strip and its components highlighted Most of the stars occupy the region in the diagram along the line called the main sequence During the stage of their lives in which stars are found on the main sequence line they are fusing hydrogen in their cores The next concentration of stars is on the horizontal branch helium fusion in the core and hydrogen burning in a shell surrounding the core Another prominent feature is the Hertzsprung gap located in the region between A5 and G0 spectral type and between 1 and 3 absolute magnitudes i e between the top of the main sequence and the giants in the horizontal branch RR Lyrae variable stars can be found in the left of this gap on a section of the diagram called the instability strip Cepheid variables also fall on the instability strip at higher luminosities The H R diagram can be used by scientists to roughly measure how far away a star cluster or galaxy is from Earth This can be done by comparing the apparent magnitudes of the stars in the cluster to the absolute magnitudes of stars with known distances or of model stars The observed group is then shifted in the vertical direction until the two main sequences overlap The difference in magnitude that was bridged in order to match the two groups is called the distance modulus and is a direct measure for the distance ignoring extinction This technique is known as main sequence fitting and is a type of spectroscopic parallax Not only the turn off in the main sequence can be used but also the tip of the red giant branch stars 8 9 The diagram seen by ESA s Gaia mission edit nbsp Hertzsprung Russell diagram showing only white dwarfs with data from ESA s Gaia mission nbsp Part of the diagram from ESA s Gaia The dark line likely represents the transition from partly convective to fully convective red dwarfs ESA s Gaia mission showed several features in the diagram that were either not known or that were suspected to exist It found a gap in the main sequence that appears for M dwarfs and that is explained with the transition from a partly convective core to a fully convective core 10 11 For white dwarfs the diagram shows several features Two main concentrations appear in this diagram following the cooling sequence of white dwarfs that are explained with the atmospheric composition of white dwarfs especially hydrogen versus helium dominated atmospheres of white dwarfs 12 A third concentration is explained with core crystallization of the white dwarfs interior This releases energy and delays the cooling of white dwarfs 13 14 Role in the development of stellar physics editSee also Stellar nucleosynthesis nbsp HR diagrams for two open clusters M67 and NGC 188 showing the main sequence turn off at different ages Contemplation of the diagram led astronomers to speculate that it might demonstrate stellar evolution the main suggestion being that stars collapsed from red giants to dwarf stars then moving down along the line of the main sequence in the course of their lifetimes Stars were thought therefore to radiate energy by converting gravitational energy into radiation through the Kelvin Helmholtz mechanism This mechanism resulted in an age for the Sun of only tens of millions of years creating a conflict over the age of the Solar System between astronomers and biologists and geologists who had evidence that the Earth was far older than that This conflict was only resolved in the 1930s when nuclear fusion was identified as the source of stellar energy Following Russell s presentation of the diagram to a meeting of the Royal Astronomical Society in 1912 Arthur Eddington was inspired to use it as a basis for developing ideas on stellar physics In 1926 in his book The Internal Constitution of the Stars he explained the physics of how stars fit on the diagram 15 The paper anticipated the later discovery of nuclear fusion and correctly proposed that the star s source of power was the combination of hydrogen into helium liberating enormous energy This was a particularly remarkable intuitive leap since at that time the source of a star s energy was still unknown thermonuclear energy had not been proven to exist and even that stars are largely composed of hydrogen see metallicity had not yet been discovered Eddington managed to sidestep this problem by concentrating on the thermodynamics of radiative transport of energy in stellar interiors 16 Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives In the 1930s and 1940s with an understanding of hydrogen fusion came an evidence backed theory of evolution to red giants following which were speculated cases of explosion and implosion of the remnants to white dwarfs The term supernova nucleosynthesis is used to describe the creation of elements during the evolution and explosion of a pre supernova star a concept put forth by Fred Hoyle in 1954 17 The pure mathematical quantum mechanics and classical mechanical models of stellar processes enable the Hertzsprung Russell diagram to be annotated with known conventional paths known as stellar sequences there continue to be added rarer and more anomalous examples as more stars are analysed and mathematical models considered See also editAsymptotic giant branch Stars powered by fusion of hydrogen and helium in shell with an inactive core of carbon and oxygen Galaxy color magnitude diagram Chart depicting the relationship between brightness and mass of large star systems Hayashi track Luminosity temperature relationship in stars Henyey track path taken by pre main sequence stars in the Hertzsprung Russell diagramPages displaying wikidata descriptions as a fallback Hess diagram Diagram of stars in astronomy Red clump Clustering of stars in astronomy diagram Stellar birthline Construct in astrophysics Stellar isochrone Curve on the Hertzsprung Russell diagram representing stars of a particular age Stellar classification Classification of stars based on spectral properties Tip of the red giant branch Primary distance indicator used in astronomy Color color diagram Astronomical diagram graphing two colour indicesReferences edit A C Maury E C Pickering 1897 Spectra of bright stars photographed with the 11 inch Draper Telescope as part of the Henry Draper Memorial Annals of Harvard College Observatory 28 1 128 Bibcode 1897AnHar 28 1M Hertzprung Ejnar 1908 Uber die Sterne der Unterabteilung c und ac nach der Spektralklassifikation von Antonia C Maury Astronomische Nachrichten 179 24 373 380 Bibcode 1909AN 179 373H doi 10 1002 asna 19081792402 a b Rosenberg Hans 1910 Uber den Zusammenhang von Helligkeit und Spektraltypus in den Plejaden Astronomische Nachrichten 186 5 71 78 Bibcode 1910AN 186 71R doi 10 1002 asna 19101860503 Vandenberg D A Brogaard K Leaman R Casagrande L 2013 The Ages of 95 Globular Clusters as Determined Using an Improved D V T O H B displaystyle Delta V TO HB nbsp Method Along with Color Magnitude Diagram Constraints and Their Implications for Broader Issues The Astrophysical Journal 775 2 134 arXiv 1308 2257 Bibcode 2013ApJ 775 134V doi 10 1088 0004 637X 775 2 134 S2CID 117065283 a b Hertzsprung E 1911 Uber die Verwendung Photographischer Effektiver Wellenlaengen zur Bestimmung von Farbenaequivalenten Publikationen des Astrophysikalischen Observatoriums zu Potsdam 22 Bd 1 Stuck Nr 63Hertzsprung E 1911 On the Use of Photographic Effective Wavelengths for the Determination of Color Equivalents Publications of the Astrophysical Observatory in Potsdam 1 22 63 Russell Henry Norris 1914 Relations Between the Spectra and Other Characteristics of the Stars Popular Astronomy 22 275 294 Bibcode 1914PA 22 275R Palma Christopher 2016 The Hertzsprung Russell Diagram ASTRO 801 Planets Stars Galaxies and the Universe John A Dutton e Education Institute College of Earth and Mineral Sciences The Pennsylvania State University Retrieved 2017 01 29 The quantities that are easiest to measure are color and magnitude so most observers refer to the diagram as a Color Magnitude diagram or CMD rather than an HR diagram Da Costa G S Armandroff T E July 1990 Standard globular cluster giant branches in the MI V I O plane Astronomical Journal 100 162 181 Bibcode 1990AJ 100 162D doi 10 1086 115500 ISSN 0004 6256 Muller Oliver Rejkuba Marina Jerjen Helmut July 2018 Tip of the Red Giant Branch Distances to the Dwarf Galaxies Dw1335 29 and Dw1340 30 in the Centaurus Group Astronomy amp Astrophysics 615 A96 arXiv 1803 02406 Bibcode 2018A amp A 615A 96M doi 10 1051 0004 6361 201732455 S2CID 67754889 Mind the Gap Gaia Mission Reveals the Insides of Stars Sky amp Telescope 2018 08 06 Retrieved 2020 02 19 Jao Wei Chun Henry Todd J Gies Douglas R Hambly Nigel C July 2018 A Gap in the Lower Main Sequence Revealed by Gaia Data Release 2 Astrophysical Journal Letters 861 1 L11 arXiv 1806 07792 Bibcode 2018ApJ 861L 11J doi 10 3847 2041 8213 aacdf6 ISSN 0004 637X S2CID 119331483 Collaboration Gaia Babusiaux C van Leeuwen F Barstow M A Jordi C Vallenari A Bossini D Bressan A Cantat Gaudin T van Leeuwen M Brown A G A August 2018 Gaia Data Release 2 Observational Hertzsprung Russell diagrams Astronomy amp Astrophysics 616 A10 arXiv 1804 09378 Bibcode 2018A amp A 616A 10G doi 10 1051 0004 6361 201832843 ISSN 0004 6361 ESA Science amp Technology Gaia reveals how Sun like stars turn solid after their demise sci esa int Retrieved 2020 02 19 Tremblay Pier Emmanuel Fontaine Gilles Fusillo Nicola Pietro Gentile Dunlap Bart H Gansicke Boris T Hollands Mark A Hermes J J Marsh Thomas R Cukanovaite Elena Cunningham Tim January 2019 Core crystallization and pile up in the cooling sequence of evolving white dwarfs Nature 565 7738 202 205 arXiv 1908 00370 Bibcode 2019Natur 565 202T doi 10 1038 s41586 018 0791 x ISSN 0028 0836 PMID 30626942 S2CID 58004893 Eddington A S Oct 1920 The Internal Constitution of the Stars The Scientific Monthly 11 4 297 303 Bibcode 1920SciMo 11 297E doi 10 1126 science 52 1341 233 JSTOR 6491 PMID 17747682 Eddington A S 1916 On the radiative equilibrium of the stars Monthly Notices of the Royal Astronomical Society 77 16 35 Bibcode 1916MNRAS 77 16E doi 10 1093 mnras 77 1 16 Hoyle F 1954 On Nuclear Reactions Occurring in Very Hot Stars I the Synthesis of Elements from Carbon to Nickel Astrophysical Journal Supplement 1 121 Bibcode 1954ApJS 1 121H doi 10 1086 190005 Bibliography edit Casagrande L Portinari L Flynn C November 2006 Accurate fundamental parameters for lower main sequence stars MNRAS 373 1 13 44 arXiv astro ph 0608504 Bibcode 2006MNRAS 373 13C doi 10 1111 j 1365 2966 2006 10999 x S2CID 16400466 Porter Roy 2003 The Cambridge History of Science Cambridge UK Cambridge University Press p 518 ISBN 978 0 521 57243 9 Sekiguchi Maki Fukugita Masataka August 2000 A Study of the B V Color Temperature Relation The Astronomical Journal 120 2 1072 1084 arXiv astro ph 9904299 Bibcode 2000AJ 120 1072S doi 10 1086 301490 S2CID 14679334 Retrieved 2008 09 14 Smith Robert 1995 Observational Astrophysics Cambridge UK Cambridge University Press p 236 ISBN 978 0 521 27834 8 External links edit nbsp Wikimedia Commons has media related to Hertzsprung Russell diagram Omega Cen H R animation of a Hertzsprung Russell diagram created from real Hubble data JavaHRD an interactive Hertzsprung Russell diagram as a Java applet BaSTI a Bag of Stellar Tracks and Isochrones simulations with FRANEC code by Teramo Astronomical Observatory Leos Ondra The first Hertzsprung Russell diagram Who first published a Hertzsprung Russell diagram Hertzsprung or Russell Answer neither Archived 2021 05 15 at the Wayback Machine Portals nbsp Astronomy nbsp Spaceflight nbsp Outer space nbsp Solar System nbsp Science Retrieved from https en wikipedia org w index php title Hertzsprung Russell diagram amp oldid 1223389562, wikipedia, wiki, book, books, library,

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