Jump to content

Instability strip: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
→Pulsations: Add a ref and comments
some more references
Line 1: Line 1:
{{Short description|Region of an astronomical diagram}}
{{Short description|Region of an astronomical diagram}}
{{For|the '''S Doradus Instability Strip'''|Luminous blue variable}}
{{For|the '''S Doradus Instability Strip'''|Luminous blue variable}}
{{Refimprove|date=November 2009}}


[[Image:HR-diag-instability-strip.svg|right|350px]]
[[Image:HR-diag-instability-strip.svg|right|350px]]
Line 10: Line 9:
== Position on the HR diagram ==
== Position on the HR diagram ==
[[File:HR Diagram for pulsating stars.svg|thumb|left|[[HR diagram]] for [[pulsating star]]s]]
[[File:HR Diagram for pulsating stars.svg|thumb|left|[[HR diagram]] for [[pulsating star]]s]]
The [[Hertzsprung–Russell diagram]] plots the real [[luminosity]] of stars against their [[effective temperature]] (their [[color]], given by the temperature of their [[photosphere]]). The instability strip intersects the [[main sequence]], (the prominent diagonal band that runs from the upper left to the lower right) in the region of A and F stars (1–2 [[Sun|solar]] mass ({{Solar mass|link=y}})) and extends to G and early K bright supergiants (early M if RV Tauri stars at minimum are included). Above the main sequence, the vast majority of stars in the instability strip are variable. Where the instability strip intersects the main sequence, the vast majority of stars are stable, but there are some variables, including the roAp stars.
The [[Hertzsprung–Russell diagram]] plots the real [[luminosity]] of stars against their [[effective temperature]] (their [[color]], given by the temperature of their [[photosphere]]). The instability strip intersects the [[main sequence]], (the prominent diagonal band that runs from the upper left to the lower right) in the region of A and F stars (1–2 [[Sun|solar]] mass ({{Solar mass|link=y}})) and extends to G and early K bright supergiants (early M if RV Tauri stars at minimum are included). Above the main sequence, the vast majority of stars in the instability strip are variable. Where the instability strip intersects the main sequence, the vast majority of stars are stable, but there are some variables, including the roAp stars.<ref name="Warner1992">{{cite book | editor = Brian Warner | date = 1992 | title = Variable Stars and Galaxies: A Symposium in Honour of Professor Michael W. Feast on His Retirement from the Directorship of the South African Astronomical Observatory, Held at the University of Cape Town, 5-7 February 1992 | publisher = Astronomical Society of the Pacific | pages = | isbn = 978-0-937707-49-4 | oclc = 1166923794 | url = https://books.google.com/books?id=y4XvAAAAMAAJ}}</ref>


==Pulsations==
==Pulsations==
Stars in the instability strip pulsate due to [[Helium|He]] III (doubly [[Ionization|ionized]] helium),<ref name=pulsations/> in a process based on the [[Kappa–mechanism]]. In normal A-F-G class stars, He is neutral in the stellar [[photosphere]]. Deeper below the photosphere, where the temperature reaches 25,000–30,000&nbsp;K, begins the He II layer (first He ionization). Second ionization of helium (He III) starts at 35,000–50,000&nbsp;K.
Stars in the instability strip pulsate due to [[Helium|He]] III (doubly [[Ionization|ionized]] helium),<ref name=pulsations/> in a process based on the [[Kappa–mechanism]]. In normal A-F-G class stars, He is neutral in the stellar [[photosphere]]. Deeper below the photosphere, where the temperature reaches 25,000–{{val|fmt=commas|30,000|ul=K}}, begins the He II layer (first He ionization). Second ionization of helium (He III) starts at 35,000–{{val|fmt=commas|50,000|u=K}}.


When the star contracts, the [[density]] and [[temperature]] of the He II layer increases. He II starts to transform into He III (second [[ionization]]). This causes the [[Opacity (optics)|opacity]] of the star to increase and the [[energy flux]] from the interior of the star is effectively absorbed. The temperature of the star rises and it begins to expand. After expansion, He III begins to recombine into He II and the opacity of the star drops. This lowers the surface temperature of the star. The outer layers contract and the cycle starts from the beginning.<ref>{{cite book
When the star contracts, the [[density]] and [[temperature]] of the He II layer increases. He II starts to transform into He III (second [[ionization]]). This causes the [[Opacity (optics)|opacity]] of the star to increase and the [[energy flux]] from the interior of the star is effectively absorbed. The temperature of the star rises and it begins to expand. After expansion, He III begins to recombine into He II and the opacity of the star drops. This lowers the surface temperature of the star. The outer layers contract and the cycle starts from the beginning.<ref>{{cite book
Line 19: Line 18:
| first=Andrew | last=Norton | year=2021
| first=Andrew | last=Norton | year=2021
| page=185 | isbn=9781000383911 | publisher=CRC Press
| page=185 | isbn=9781000383911 | publisher=CRC Press
| url=https://www.google.com/books/edition/Understanding_the_Universe/N1kkEAAAQBAJ?pg=PA185 }}</ref> In some stars, the pulsations are caused by the opacity peak of metal ions at about {{val|fmt=commas|200,000|u=K}}.<ref name="TakeutiBuchler2012">{{cite book | editor1 = Mine Takeuti | editor2 = J. Robert Buchler | date = 6 December 2012 | title = Nonlinear Phenomena in Stellar Variability | publisher = Springer Science & Business Media | pages = 70– | isbn = 9789401110624 | oclc = 1243544743 | url = https://books.google.com/books?id=cSnSuzGgPJ0C&pg=PA70}}</ref>
| url=https://www.google.com/books/edition/Understanding_the_Universe/N1kkEAAAQBAJ?pg=PA185 }}</ref>


The phase shift between a star's [[radius|radial]] pulsations and [[Apparent magnitude|brightness]] variations depends on the distance of He II zone from the stellar surface in the [[stellar atmosphere]]. For most Cepheids, this creates a distinctly asymmetrical observed light curve, rising rapidly to maximum and falling slowly back down to minimum.
The phase shift between a star's [[radius|radial]] pulsations and [[Apparent magnitude|brightness]] variations depends on the distance of He II zone from the stellar surface in the [[stellar atmosphere]]. For most Cepheids, this creates a distinctly asymmetrical observed light curve, rising rapidly to maximum and falling slowly back down to minimum.<ref name="LooreDoom2012">{{cite book | author1 = C. de Loore | author2 = C. Doom | date = 6 December 2012 | title = Structure and Evolution of Single and Binary Stars | publisher = Springer Science & Business Media | pages = 232– | isbn = 9789401125024 | url = https://books.google.com/books?id=Zp7qCAAAQBAJ&pg=PA232}}</ref>


==Other pulsating stars==
==Other pulsating stars==
There are several types of pulsating star not found on the instability strip and with pulsations driven by different mechanisms. At cooler temperatures are the [[long period variable]] [[Asymptotic giant branch|AGB]] stars. At hotter temperatures are the [[Beta Cephei variable|Beta Cephei]] and [[PV Telescopii variable|PV Telescopii]] variables. Right at the edge of the instability strip near the main sequence are [[Gamma Doradus variables]]. The band of [[White dwarfs]] has three separate regions and types of variable: DOV, DBV, and DAV (= [[ZZ Ceti variables]]) white dwarfs. Each of these types of pulsating variable has an associated instability strip<ref name=v777>{{Cite journal | last1 = Beauchamp | first1 = A. | last2 = Wesemael | first2 = F. | last3 = Bergeron | first3 = P. | last4 = Fontaine | first4 = G. | last5 = Saffer | first5 = R. A. | last6 = Liebert | first6 = James | last7 = Brassard | first7 = P. | doi = 10.1086/307148 | title = Spectroscopic Studies of DB White Dwarfs: The Instability Strip of the Pulsating DB (V777 Herculis) Stars | journal = The Astrophysical Journal | volume = 516 | issue = 2 | pages = 887 | year = 1999 |bibcode = 1999ApJ...516..887B | doi-access = free }}</ref><ref name=hot>{{Cite journal |author1-link=Sumner Starrfield | last1 = Starrfield | first1 = S. G. | last2 = Cox | first2 = A. N. | last3 = Hodson | first3 = S. W. | last4 = Pesnell | first4 = W. D. | title = The discovery of nonradial instability strips for hot, evolved stars | doi = 10.1086/184023 | journal = The Astrophysical Journal | volume = 268 | pages = L27 | year = 1983 |bibcode = 1983ApJ...268L..27S }}</ref><ref name=theoretical>{{Cite journal | last1 = Dupret | first1 = M. -A. | last2 = Grigahcène | first2 = A. | last3 = Garrido | first3 = R. | last4 = Gabriel | first4 = M. | last5 = Scuflaire | first5 = R. | year = 2004 | title = Theoretical instability strips for δ Scuti and γ Doradus stars | journal = Astronomy and Astrophysics | volume = 414 | issue = 2 | pages = L17 | bibcode = 2004A&A...414L..17D | doi = 10.1051/0004-6361:20031740 | doi-access = free }}</ref> created by variable opacity partial ionisation regions other than helium.<ref name=pulsations/>
There are several types of pulsating star not found on the instability strip and with pulsations driven by different mechanisms. At cooler temperatures are the [[long period variable]] [[Asymptotic giant branch|AGB]] stars. At hotter temperatures are the [[Beta Cephei variable|Beta Cephei]] and [[PV Telescopii variable|PV Telescopii]] variables. Right at the edge of the instability strip near the main sequence are [[Gamma Doradus variables]]. The band of [[White dwarfs]] has three separate regions and types of variable: DOV, DBV, and DAV (= [[ZZ Ceti variables]]) white dwarfs. Each of these types of pulsating variable has an associated instability strip<ref name=v777>{{Cite journal | last1 = Beauchamp | first1 = A. | last2 = Wesemael | first2 = F. | last3 = Bergeron | first3 = P. | last4 = Fontaine | first4 = G. | last5 = Saffer | first5 = R. A. | last6 = Liebert | first6 = James | last7 = Brassard | first7 = P. | doi = 10.1086/307148 | title = Spectroscopic Studies of DB White Dwarfs: The Instability Strip of the Pulsating DB (V777 Herculis) Stars | journal = The Astrophysical Journal | volume = 516 | issue = 2 | pages = 887 | year = 1999 |bibcode = 1999ApJ...516..887B | doi-access = free }}</ref><ref name=hot>{{Cite journal |author1-link=Sumner Starrfield | last1 = Starrfield | first1 = S. G. | last2 = Cox | first2 = A. N. | last3 = Hodson | first3 = S. W. | last4 = Pesnell | first4 = W. D. | title = The discovery of nonradial instability strips for hot, evolved stars | doi = 10.1086/184023 | journal = The Astrophysical Journal | volume = 268 | pages = L27 | year = 1983 |bibcode = 1983ApJ...268L..27S }}</ref><ref name=theoretical>{{Cite journal | last1 = Dupret | first1 = M. -A. | last2 = Grigahcène | first2 = A. | last3 = Garrido | first3 = R. | last4 = Gabriel | first4 = M. | last5 = Scuflaire | first5 = R. | year = 2004 | title = Theoretical instability strips for δ Scuti and γ Doradus stars | journal = Astronomy and Astrophysics | volume = 414 | issue = 2 | pages = L17 | bibcode = 2004A&A...414L..17D | doi = 10.1051/0004-6361:20031740 | doi-access = free }}</ref> created by variable opacity partial ionisation regions other than helium.<ref name=pulsations/>


Most high luminosity supergiants are somewhat variable, including the [[Alpha Cygni variables]]. In the specific region of more luminous stars above the instability strip are found the [[yellow hypergiant]]s which have irregular pulsations and eruptions. The hotter [[luminous blue variable]]s may be related and show similar short- and long-term [[Electromagnetic spectrum|spectral]] and brightness variations with irregular eruptions.
Most high luminosity supergiants are somewhat variable, including the [[Alpha Cygni variables]]. In the specific region of more luminous stars above the instability strip are found the [[yellow hypergiant]]s which have irregular pulsations and eruptions. The hotter [[luminous blue variable]]s may be related and show similar short- and long-term [[Electromagnetic spectrum|spectral]] and brightness variations with irregular eruptions.<ref name="CatelanSmith2015">{{cite book | author1 = Márcio Catelan | author2 = Horace A. Smith | date = 23 March 2015 | title = Pulsating Stars | publisher = John Wiley & Sons | pages = 432– | isbn = 978-3-527-40715-6 | url = https://books.google.com/books?id=tFhVDwAAQBAJ&pg=PA432}}</ref>
{{clear}}
{{clear}}


Revision as of 16:32, 25 April 2023

For the S Doradus Instability Strip, see Luminous blue variable.

The unqualified term instability strip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating variable stars:[1] Delta Scuti variables, SX Phoenicis variables, and rapidly oscillating Ap stars (roAps) near the main sequence; RR Lyrae variables where it intersects the horizontal branch; and the Cepheid variables where it crosses the supergiants.

RV Tauri variables are also often considered to lie on the instability strip, occupying the area to the right of the brighter Cepheids (at lower temperatures), since their stellar pulsations are attributed to the same mechanism.

Position on the HR diagram

HR diagram for pulsating stars

The Hertzsprung–Russell diagram plots the real luminosity of stars against their effective temperature (their color, given by the temperature of their photosphere). The instability strip intersects the main sequence, (the prominent diagonal band that runs from the upper left to the lower right) in the region of A and F stars (1–2 solar mass (M☉)) and extends to G and early K bright supergiants (early M if RV Tauri stars at minimum are included). Above the main sequence, the vast majority of stars in the instability strip are variable. Where the instability strip intersects the main sequence, the vast majority of stars are stable, but there are some variables, including the roAp stars.[2]

Pulsations

Stars in the instability strip pulsate due to He III (doubly ionized helium),[1] in a process based on the Kappa–mechanism. In normal A-F-G class stars, He is neutral in the stellar photosphere. Deeper below the photosphere, where the temperature reaches 25,000–30,000 K, begins the He II layer (first He ionization). Second ionization of helium (He III) starts at 35,000–50,000 K.

When the star contracts, the density and temperature of the He II layer increases. He II starts to transform into He III (second ionization). This causes the opacity of the star to increase and the energy flux from the interior of the star is effectively absorbed. The temperature of the star rises and it begins to expand. After expansion, He III begins to recombine into He II and the opacity of the star drops. This lowers the surface temperature of the star. The outer layers contract and the cycle starts from the beginning.[3] In some stars, the pulsations are caused by the opacity peak of metal ions at about 200,000 K.[4]

The phase shift between a star's radial pulsations and brightness variations depends on the distance of He II zone from the stellar surface in the stellar atmosphere. For most Cepheids, this creates a distinctly asymmetrical observed light curve, rising rapidly to maximum and falling slowly back down to minimum.[5]

Other pulsating stars

There are several types of pulsating star not found on the instability strip and with pulsations driven by different mechanisms. At cooler temperatures are the long period variable AGB stars. At hotter temperatures are the Beta Cephei and PV Telescopii variables. Right at the edge of the instability strip near the main sequence are Gamma Doradus variables. The band of White dwarfs has three separate regions and types of variable: DOV, DBV, and DAV (= ZZ Ceti variables) white dwarfs. Each of these types of pulsating variable has an associated instability strip[6][7][8] created by variable opacity partial ionisation regions other than helium.[1]

Most high luminosity supergiants are somewhat variable, including the Alpha Cygni variables. In the specific region of more luminous stars above the instability strip are found the yellow hypergiants which have irregular pulsations and eruptions. The hotter luminous blue variables may be related and show similar short- and long-term spectral and brightness variations with irregular eruptions.[9]

References

  1. ^ a b c Gautschy, A.; Saio, H. (1996). "Stellar Pulsations Across the HR Diagram: Part 2". Annual Review of Astronomy and Astrophysics. 34: 551. Bibcode:1996ARA&A..34..551G. doi:10.1146/annurev.astro.34.1.551.
  2. ^ Brian Warner, ed. (1992). Variable Stars and Galaxies: A Symposium in Honour of Professor Michael W. Feast on His Retirement from the Directorship of the South African Astronomical Observatory, Held at the University of Cape Town, 5-7 February 1992. Astronomical Society of the Pacific. ISBN 978-0-937707-49-4. OCLC 1166923794.
  3. ^ Norton, Andrew (2021). Understanding the Universe: The Physics of the Cosmos from Quasars to Quarks. CRC Press. p. 185. ISBN 9781000383911.
  4. ^ Mine Takeuti; J. Robert Buchler, eds. (6 December 2012). Nonlinear Phenomena in Stellar Variability. Springer Science & Business Media. pp. 70–. ISBN 9789401110624. OCLC 1243544743.
  5. ^ C. de Loore; C. Doom (6 December 2012). Structure and Evolution of Single and Binary Stars. Springer Science & Business Media. pp. 232–. ISBN 9789401125024.
  6. ^ Beauchamp, A.; Wesemael, F.; Bergeron, P.; Fontaine, G.; Saffer, R. A.; Liebert, James; Brassard, P. (1999). "Spectroscopic Studies of DB White Dwarfs: The Instability Strip of the Pulsating DB (V777 Herculis) Stars". The Astrophysical Journal. 516 (2): 887. Bibcode:1999ApJ...516..887B. doi:10.1086/307148.
  7. ^ Starrfield, S. G.; Cox, A. N.; Hodson, S. W.; Pesnell, W. D. (1983). "The discovery of nonradial instability strips for hot, evolved stars". The Astrophysical Journal. 268: L27. Bibcode:1983ApJ...268L..27S. doi:10.1086/184023.
  8. ^ Dupret, M. -A.; Grigahcène, A.; Garrido, R.; Gabriel, M.; Scuflaire, R. (2004). "Theoretical instability strips for δ Scuti and γ Doradus stars". Astronomy and Astrophysics. 414 (2): L17. Bibcode:2004A&A...414L..17D. doi:10.1051/0004-6361:20031740.
  9. ^ Márcio Catelan; Horace A. Smith (23 March 2015). Pulsating Stars. John Wiley & Sons. pp. 432–. ISBN 978-3-527-40715-6.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Instability_strip&oldid=1151690782"