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A '''Delta Scuti variable''' (sometimes termed '''dwarf cepheid''') is a subclass of young [[pulsating star]].
{{Short description|Subclass of young pulsating star}}
[[File:DeltaSctLightCurve.png|thumb|right|upright=1.25|A [[light curve]] for Delta Scuti, plotted from ''[[Hipparcos]]'' data<ref name=HIPCurve>{{cite web |title=Light Curve |url=https://www.cosmos.esa.int/web/hipparcos/java-tools/light-curve |website=Hipparcos ESA |publisher=ESA |access-date=17 February 2022}}</ref>]]
⚫
These variables as well as [[classical cepheids]] are important [[standard candles]] and have been used to establish the distance to the [[Large Magellanic Cloud]], [[globular clusters]], [[open clusters]], and the [[Galactic Center]].<ref name=mcnamara2000>{{cite journal |bibcode=2000PASP..112..202M |title=The Distance to the Galactic Center |journal=Publications of the Astronomical Society of the Pacific |volume=112 |issue=768 |pages=202 |last1=McNamara |first1=D. H. |last2=Madsen |first2=J. B. |last3=Barnes |first3=J. |last4=Ericksen |first4=B. F. |year=2000 |doi=10.1086/316512 |doi-access=free }}</ref><ref name=mcnamara2007>{{cite journal |bibcode=2007AJ....133.2752M |title=A δ Scuti Distance to the Large Magellanic Cloud |journal=The Astronomical Journal |volume=133 |issue=6 |pages=2752 |last1=McNamara |first1=D. Harold |last2=Clementini |first2=Gisella |last3=Marconi |first3=Marcella |year=2007 |doi=10.1086/513717 |arxiv=astro-ph/0702107 }}</ref><ref name=majaess2011>{{cite journal |bibcode=2011JAVSO..39..122M |title=Anchoring the Universal Distance Scale Via a Wesenheit Template |journal=Journal of the American Association of Variable Star Observers (Jaavso) |volume=39 |issue=1 |pages=122 |last1=Majaess |first1=D. J. |last2=Turner |first2=D. G. |last3=Lane |first3=D. J. |last4=Henden |first4=A. A. |last5=Krajci |first5=T. |year=2011 }}</ref><ref name=majaess2011b>{{cite journal |arxiv=1102.1705 |last1=Majaess |first1=Daniel J. |title=Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars |journal=Journal of the American Association of Variable Star Observers (Jaavso) |volume=39 |issue=2 |pages=219 |last2=Turner |first2=David G. |last3=Lane |first3=David J. |last4=Krajci |first4=Tom |year=2011 |bibcode=2011JAVSO..39..219M }}</ref> The variables follow a [[period-luminosity relation]] in certain passbands like other [[standard candles]] such as [[Cepheids]].<ref name=majaess2011/><ref name=majaess2011b/><ref name=poleski2010>{{cite journal |bibcode=2010AcA....60....1P |title=The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. VI. Delta Scuti Stars in the Large Magellanic Cloud |journal=Acta Astronomica |volume=60 |issue=1 |pages=1 |last1=Poleski |first1=R. |last2=Soszyński |first2=I. |last3=Udalski |first3=A. |last4=Szymański |first4=M. K. |last5=Kubiak |first5=M. |last6=Pietrzyński |first6=G. |last7=Wyrzykowski |first7=Ł. |last8=Szewczyk |first8=O. |last9=Ulaczyk |first9=K. |year=2010 }}</ref><ref name=cohen2012>{{cite journal |bibcode=2012MNRAS.419..342C |title=SX Phoenicis period-luminosity relations and the blue straggler connection |journal=Monthly Notices of the Royal Astronomical Society |volume=419 |issue=1 |pages=342 |last1=Cohen |first1=Roger E. |last2=Sarajedini |first2=Ata |year=2012 |doi=10.1111/j.1365-2966.2011.19697.x |doi-access=free }}</ref> [[SX Phoenicis variables]] are generally considered to be a subclass of Delta Scuti variables that contain old stars, and can be found in globular clusters. SX Phe variables also follow a period-luminosity relation.<ref name=majaess2011/><ref name=cohen2012/> The [[Rapidly oscillating Ap stars]] are also a subclass of Delta Scuti variables, found on the main sequence.<ref name=kopacki2003>{{cite journal |bibcode=2003A&A...398..541K |title=Variable stars in the globular cluster M 13 |journal=Astronomy and Astrophysics |volume=398 |pages=541–550 |last1=Kopacki |first1=G. |last2=Kołaczkowski |first2=Z. |last3=Pigulski |first3=A. |year=2003 |arxiv=astro-ph/0211042 |doi=10.1051/0004-6361:20021624 }}</ref> One last sub-class are the pre-main sequence (PMS) Delta Scuti variables.
A '''Delta Scuti variable''' (sometimes termed '''dwarf cepheid''' when the V-band amplitude is larger than 0.3 mag.) is a subclass of young [[pulsating star]].
⚫
These variables as well as [[classical cepheids]] are important [[standard candles]] and have been used to establish the distance to the [[Large Magellanic Cloud]], [[globular clusters]], [[open clusters]], and the [[Galactic Center]].<ref name=mcnamara2000>{{cite journal |bibcode=2000PASP..112..202M |title=The Distance to the Galactic Center |journal=Publications of the Astronomical Society of the Pacific |volume=112 |issue=768 |pages=202 |last1=McNamara |first1=D. H. |author-link1=D. Harold McNamara |last2=Madsen |first2=J. B. |last3=Barnes |first3=J. |last4=Ericksen |first4=B. F. |year=2000 |doi=10.1086/316512 |doi-access=free }}</ref><ref name=mcnamara2007>{{cite journal |bibcode=2007AJ....133.2752M |title=A δ Scuti Distance to the Large Magellanic Cloud |journal=The Astronomical Journal |volume=133 |issue=6 |pages=2752–2763 |last1=McNamara |first1=D. Harold |author-link1=D. Harold McNamara |last2=Clementini |first2=Gisella |last3=Marconi |first3=Marcella |year=2007 |doi=10.1086/513717 |arxiv=astro-ph/0702107 |s2cid=18053647 }}</ref><ref name=majaess2011>{{cite journal |bibcode=2011JAVSO..39..122M |title=Anchoring the Universal Distance Scale Via a Wesenheit Template |journal=Journal of the American Association of Variable Star Observers (Jaavso) |volume=39 |issue=1 |pages=122 |last1=Majaess |first1=D. J. |last2=Turner |first2=D. G. |last3=Lane |first3=D. J. |last4=Henden |first4=A. A. |last5=Krajci |first5=T. |year=2011 |arxiv=1007.2300 }}</ref><ref name=majaess2011b>{{cite journal |arxiv=1102.1705 |last1=Majaess |first1=Daniel J. |title=Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars |journal=Journal of the American Association of Variable Star Observers (Jaavso) |volume=39 |issue=2 |pages=219 |last2=Turner |first2=David G. |last3=Lane |first3=David J. |last4=Krajci |first4=Tom |year=2011 |bibcode=2011JAVSO..39..219M }}</ref> The variables follow a [[period-luminosity relation]] in certain passbands like other [[standard candles]] such as [[Cepheids]].<ref name=majaess2011/><ref name=majaess2011b/><ref name=poleski2010>{{cite journal |bibcode=2010AcA....60....1P |title=The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. VI. Delta Scuti Stars in the Large Magellanic Cloud |journal=Acta Astronomica |volume=60 |issue=1 |pages=1 |last1=Poleski |first1=R. |last2=Soszyński |first2=I. |last3=Udalski |first3=A. |last4=Szymański |first4=M. K. |last5=Kubiak |first5=M. |last6=Pietrzyński |first6=G. |last7=Wyrzykowski |first7=Ł. |last8=Szewczyk |first8=O. |last9=Ulaczyk |first9=K. |year=2010 |arxiv=1004.0950 }}</ref><ref name=cohen2012>{{cite journal |bibcode=2012MNRAS.419..342C |title=SX Phoenicis period-luminosity relations and the blue straggler connection |journal=Monthly Notices of the Royal Astronomical Society |volume=419 |issue=1 |pages=342 |last1=Cohen |first1=Roger E. |last2=Sarajedini |first2=Ata |year=2012 |doi=10.1111/j.1365-2966.2011.19697.x |doi-access=free }}</ref> [[SX Phoenicis variables]] are generally considered to be a subclass of Delta Scuti variables that contain old stars, and can be found in globular clusters. SX Phe variables also follow a period-luminosity relation.<ref name=majaess2011/><ref name=cohen2012/> One last sub-class are the pre-main sequence (PMS) Delta Scuti variables.


The [[OGLE]] and [[MACHO]] surveys have detected nearly 3000 Delta Scuti variables in the [[Large Magellanic Cloud]].<ref name=poleski2010/><ref name=garg2010>{{cite journal |bibcode=2010AJ....140..328G |title=High-amplitude δ-Scutis in the Large Magellanic Cloud |journal=The Astronomical Journal |volume=140 |issue=2 |pages=328 |last1=Garg |first1=A. |last2=Cook |first2=K. H. |last3=Nikolaev |first3=S. |last4=Huber |first4=M. E. |last5=Rest |first5=A. |last6=Becker |first6=A. C. |last7=Challis |first7=P. |last8=Clocchiatti |first8=A. |last9=Miknaitis |first9=G. |last10=Minniti |first10=D. |last11=Morelli |first11=L. |last12=Olsen |first12=K. |last13=Prieto |first13=J. L. |last14=Suntzeff |first14=N. B. |last15=Welch |first15=D. L. |last16=Wood-Vasey |first16=W. M. |year=2010 |doi=10.1088/0004-6256/140/2/328 |hdl=1969.1/181688 |hdl-access=free }}</ref> Typical brightness fluctuations are from 0.003 to 0.9 [[apparent magnitude|magnitude]]s in [[color index|V]] over a period of a few hours, although the [[amplitude]] and [[orbital period|period]] of the fluctuations can vary greatly. The stars are usually A0 to F5 [[stellar classification|type]] [[giant star|giant]] or [[main sequence]] stars. The high-amplitude Delta Scuti variables are also called '''AI Velorum stars'''. They are the second most abundant variable source in the Milky Way after white dwarfs.
The [[OGLE]] and [[MACHO]] surveys have detected nearly 3000 Delta Scuti variables in the [[Large Magellanic Cloud]].<ref name=poleski2010/><ref name=garg2010>{{cite journal |bibcode=2010AJ....140..328G |title=High-amplitude δ-Scutis in the Large Magellanic Cloud |journal=The Astronomical Journal |volume=140 |issue=2 |pages=328 |last1=Garg |first1=A. |last2=Cook |first2=K. H. |last3=Nikolaev |first3=S. |last4=Huber |first4=M. E. |last5=Rest |first5=A. |last6=Becker |first6=A. C. |last7=Challis |first7=P. |last8=Clocchiatti |first8=A. |last9=Miknaitis |first9=G. |last10=Minniti |first10=D. |last11=Morelli |first11=L. |last12=Olsen |first12=K. |last13=Prieto |first13=J. L. |last14=Suntzeff |first14=N. B. |last15=Welch |first15=D. L. |last16=Wood-Vasey |first16=W. M. |year=2010 |doi=10.1088/0004-6256/140/2/328 |arxiv=1004.0955 |hdl=1969.1/181688 |s2cid=118386274 |hdl-access=free }}</ref> Typical brightness fluctuations are from 0.003 to 0.9 [[apparent magnitude|magnitude]]s in [[color index|V]] over a period of a few hours, although the [[amplitude]] and [[orbital period|period]] of the fluctuations can vary greatly. The stars are usually A0 to F5 [[stellar classification|type]] [[giant star|giant]] or [[main sequence]] stars. The high-amplitude Delta Scuti variables are also called '''AI Velorum stars''', after the prototype [[AI Velorum]].


Delta Scuti stars exhibit both radial and non-radial luminosity pulsations. Non-radial pulsations are when some parts of the surface move inwards and some outward at the same time. Radial pulsations are a special case, where the star expands and contracts around its equilibrium state by altering the radius to maintain its spherical shape. The variations are due to the swelling and shrinking of the star through the Eddington Valve or [[Kappa-mechanism]]. The stars have a helium rich atmosphere. As helium is heated it becomes more ionised, which is more opaque. So at the dimmest part in the cycle the star has highly ionised opaque helium in its atmosphere blocking part of the light from escaping. The energy from this “blocked light” causes the helium to heat up, expand, ionise, become more transparent and therefore allow more light through. As more light is let through the star appears brighter and, with the expansion, the helium begins to cool down. Hence the helium contracts and heats up again and the cyclical process continues. Throughout their lifetime Delta Scuti stars exhibit pulsation when they are situated on the classical Cepheid [[instability strip]]. They then move across from the main sequence into the giant branch.
Delta Scuti stars exhibit both radial and non-radial luminosity pulsations. Non-radial pulsations are when some parts of the surface move inwards and some outward at the same time. Radial pulsations are a special case, where the star expands and contracts around its equilibrium state by altering the radius to maintain its spherical shape. The variations are due to the swelling and shrinking of the star through the Eddington Valve or [[Kappa-mechanism]]. The stars have a helium rich atmosphere. As helium is compressed it becomes more ionised, which is more opaque. So at the dimmest part in the cycle the star has highly ionised opaque helium in its atmosphere blocking part of the light from escaping. The energy from this “blocked light” causes the helium to heat up then expand, become more transparent and therefore allow more light through. As more light is let through the star appears brighter and, with the expansion, the helium begins to cool down. Hence the helium contracts under gravity and heats up again and the cyclical process continues. Throughout their lifetime Delta Scuti stars exhibit pulsation when they are situated on the classical Cepheid [[instability strip]]. They then move across from the main sequence into the giant branch.


The prototype of these sorts of variable stars is [[Delta Scuti]] (δ Sct), which exhibits brightness fluctuations from +4.60 to +4.79 in [[apparent magnitude]] with a period of 4.65 hours. Other well known Delta Scuti variables include [[Altair]], [[Denebola]] (β Leonis) and [[Beta Cassiopeiae|β Cassiopeiae]]. [[Vega]] (α Lyrae) is a suspected Delta Scuti variable,<ref>{{citation | display-authors=1 | last1=I.A. | first1=Vasil'yev | last2=Merezhin | first2=V. P. | last3=Nalimov | first3=V. N. | last4=Novosyolov | first4=V. A. | url=http://www.konkoly.hu/pub/ibvs/3301/3308.txt | title=On the Variability of Vega | date=1989-03-17 | publisher=Commission 27 of the I.A.U | accessdate=2007-10-30 }}</ref> but this remains unconfirmed.
The prototype of these sorts of variable stars is [[Delta Scuti]] (δ Sct), which exhibits brightness fluctuations from +4.60 to +4.79 in [[apparent magnitude]] with a period of 4.65 hours. Other well known Delta Scuti variables include [[Altair]] and [[Denebola]] (β Leonis). [[Vega]] (α Lyrae) is a suspected Delta Scuti variable,<ref>{{cite web | display-authors=1 | last1=I.A. | first1=Vasil'yev | last2=Merezhin | first2=V. P. | last3=Nalimov | first3=V. N. | last4=Novosyolov | first4=V. A. | url=http://www.konkoly.hu/pub/ibvs/3301/3308.txt | title=On the Variability of Vega | date=1989-03-17 | publisher=Commission 27 of the I.A.U | access-date=2007-10-30 }}</ref> but this remains unconfirmed.


==Examples==
==Examples==
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{| class="wikitable sortable" style="font-size:90%;"
{| class="wikitable sortable" style="font-size:90%;"
|- bgcolor="#efefef"
|- bgcolor="#efefef"
! width="10%"|'''Designation (name)'''
! width="15%"|'''Designation (name)'''
! width="10%"|'''Constellation'''
! width="15%"|'''Discovery'''
! width="15%"|'''Discovery'''
! width="8%"|''[[Apparent magnitude]]'' (Maximum)<ref name="ReferenceA">''(visual magnitude, unless marked'' (B) ''(= blue) or'' (p) ''(= photographic))''</ref>
! width="8%"|''Maximum''<ref name="ReferenceA">''(apparent visual magnitude''</ref> ([[Apparent magnitude|magnitude]])
! width="8%"|''[[Apparent magnitude]]'' (Minimum)<ref name="ReferenceA"/>
! width="8%"|''Minimum''<ref name="ReferenceA"/> ([[Apparent magnitude|magnitude]])
! width="8%"|''Range of magnitude''
! width="8%"|''Range of magnitude''
! width="11%"|'''Period'''
! width="11%"|'''Period'''
! width="15%"|'''Spectral type'''
! width="15%"|'''Spectral type'''
! width="15%"|'''Comment'''
! width="25%"|'''Comment'''
|---
|---
| [[Gamma Boötis]]
| [[γ Boötis]]
⚫
| [[Boötes]]
|
|
| {{ntsh|3.02}}3<sup>m</sup>.02
| style="text-align:right; padding-right: 1em;" | {{ntsh|3.02}}3.02
| {{ntsh|3.07}}3<sup>m</sup>.07
| style="text-align:right; padding-right: 1em;" | {{ntsh|3.07}}3.07
| {{nts|0.05}}
| style="text-align:right; padding-right: 1em;" | {{nts|0.05}}
| {{nts|6.96}}&nbsp;h
| style="text-align:right; padding-right: 1em;" | {{nts|6.96}}&nbsp;h
|bgcolor="{{Color temperature|7800|hexval}}"| A7III
| A7III
|
|
|---
|---
| [[Epsilon Cephei]]
| [[ε Cephei]]
| [[Cepheus (constellation)|Cepheus]]
|
|
| {{ntsh|4.15}}4<sup>m</sup>.15
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.15}}4.15
| {{ntsh|4.21}}4<sup>m</sup>.21
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.21}}4.21
| {{nts|0.06}}
| style="text-align:right; padding-right: 1em;" | {{nts|0.06}}
| {{nts|0.98}}&nbsp;h
| style="text-align:right; padding-right: 1em;" | {{nts|0.98}}&nbsp;h
|bgcolor="{{Color temperature|7514|hexval}}"| F0IV
| F0IV
|
|
|---
|---
| [[Delta Scuti]]
| [[HD 40372]]
| [[Scutum (constellation)|Scutum]]
|
|
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.88}}5.88
| {{ntsh|4.6}}4<sup>m</sup>.6
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.92 }}5.92
| {{ntsh|4.79}}4<sup>m</sup>.79
| style="text-align:right; padding-right: 1em;" | {{nts|0.04}}
| {{nts|0.19}}
| {{nts|4.65}}&nbsp;h
| style="text-align:right; padding-right: 1em;" | {{nts|1.466}}&nbsp;h
|bgcolor="{{Color temperature|7706|hexval}}"| A5me
| F2 IIIp
| In eclipsing binary system
|---
| [[α Lyrae]] (Vega)
|
| style="text-align:right; padding-right: 1em;" | {{ntsh|-0.02}}−0.02
| style="text-align:right; padding-right: 1em;" | {{ntsh|0.07}}0.07
| style="text-align:right; padding-right: 1em;" | {{nts|0.03}}
| style="text-align:right; padding-right: 1em;" | {{nts|2.57}}&nbsp;h
|bgcolor="{{Color temperature|9602|hexval}}"| A0Va
| 5th brightest star in the night sky
|---
⚫
| [[HR 1170]]
|
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.77}}5.77
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.91}}5.91
| style="text-align:right; padding-right: 1em;" | {{nts|0.14}}
| style="text-align:right; padding-right: 1em;" | {{nts|2.39}}&nbsp;h
|bgcolor="{{Color temperature|7194|hexval}}"| A9IV
|
|---
| [[δ Scuti]]
|
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.6}}4.60
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.79}}4.79
| style="text-align:right; padding-right: 1em;" | {{nts|0.19}}
| style="text-align:right; padding-right: 1em;" | {{nts|4.65}}&nbsp;h
|bgcolor="{{Color temperature|6638|hexval}}"| F2 IIIp
| prototype
| prototype
|---
| [[V701 Coronae Australis]]
| Lampens & Rufuen (1990)
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.69}}5.69
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.73}}5.73
| style="text-align:right; padding-right: 1em;" | {{nts|0.04}}
| style="text-align:right; padding-right: 1em;" | {{nts|3.25}}&nbsp;h
|bgcolor="{{Color temperature|7046|hexval}}"| F2 III/IV
|
|---
|---
| [[QQ Telescopii]]
| Kurtz (1982)
| style="text-align:right; padding-right: 1em;" | {{ntsh|6.53}}6.53 (blue)
| style="text-align:right; padding-right: 1em;" | {{ntsh|6.58}}6.58 (blue)
| style="text-align:right; padding-right: 1em;" | {{nts|0.05}}
| style="text-align:right; padding-right: 1em;" | {{nts|1.52}}&nbsp;h
|bgcolor={{Color temperature|7380|hexval}}| F2 IV
|
|---
|---
|}
|}


Other examples include - [[Sigma Octantis]] and [[Beta Cassiopeiae]]
Other examples include - [[σ Octantis]] and [[β Cassiopeiae]]


==References==
==References==
{{reflist}}
{{Reflist}}

==Further reading==
*Samus N.N., Durlevich O.V., et al. ''Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)''
*Samus N.N., Durlevich O.V., et al. ''Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)''
*[http://www.daviddarling.info/encyclopedia/A/AI_Velorum_star.html AI Velorum star] at The Encyclopedia of Astrobiology, Astronomy, and Spaceflight
*[http://www.daviddarling.info/encyclopedia/A/AI_Velorum_star.html AI Velorum star] at The Encyclopedia of Astrobiology, Astronomy, and Spaceflight
Line 63: Line 109:


{{Variable star topics}}
{{Variable star topics}}
{{Authority control}}


[[Category:Cepheid variables]]
[[Category:Cepheid variables]]
[[Category:Delta Scuti variables|*]]
[[Category:Delta Scuti variables|*]]
[[Category:Stellar physics]]

Latest revision as of 03:21, 6 July 2024

A light curve for Delta Scuti, plotted from Hipparcos data[1]

A Delta Scuti variable (sometimes termed dwarf cepheid when the V-band amplitude is larger than 0.3 mag.) is a subclass of young pulsating star. These variables as well as classical cepheids are important standard candles and have been used to establish the distance to the Large Magellanic Cloud, globular clusters, open clusters, and the Galactic Center.[2][3][4][5] The variables follow a period-luminosity relation in certain passbands like other standard candles such as Cepheids.[4][5][6][7] SX Phoenicis variables are generally considered to be a subclass of Delta Scuti variables that contain old stars, and can be found in globular clusters. SX Phe variables also follow a period-luminosity relation.[4][7] One last sub-class are the pre-main sequence (PMS) Delta Scuti variables.

The OGLE and MACHO surveys have detected nearly 3000 Delta Scuti variables in the Large Magellanic Cloud.[6][8] Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude and period of the fluctuations can vary greatly. The stars are usually A0 to F5 type giant or main sequence stars. The high-amplitude Delta Scuti variables are also called AI Velorum stars, after the prototype AI Velorum.

Delta Scuti stars exhibit both radial and non-radial luminosity pulsations. Non-radial pulsations are when some parts of the surface move inwards and some outward at the same time. Radial pulsations are a special case, where the star expands and contracts around its equilibrium state by altering the radius to maintain its spherical shape. The variations are due to the swelling and shrinking of the star through the Eddington Valve or Kappa-mechanism. The stars have a helium rich atmosphere. As helium is compressed it becomes more ionised, which is more opaque. So at the dimmest part in the cycle the star has highly ionised opaque helium in its atmosphere blocking part of the light from escaping. The energy from this “blocked light” causes the helium to heat up then expand, become more transparent and therefore allow more light through. As more light is let through the star appears brighter and, with the expansion, the helium begins to cool down. Hence the helium contracts under gravity and heats up again and the cyclical process continues. Throughout their lifetime Delta Scuti stars exhibit pulsation when they are situated on the classical Cepheid instability strip. They then move across from the main sequence into the giant branch.

The prototype of these sorts of variable stars is Delta Scuti (δ Sct), which exhibits brightness fluctuations from +4.60 to +4.79 in apparent magnitude with a period of 4.65 hours. Other well known Delta Scuti variables include Altair and Denebola (β Leonis). Vega (α Lyrae) is a suspected Delta Scuti variable,[9] but this remains unconfirmed.

Examples

[edit]
This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.
Designation (name) Discovery Maximum[10] (magnitude) Minimum[10] (magnitude) Range of magnitude Period Spectral type Comment
γ Boötis 3.02 3.07 0.05 6.96 h A7III
ε Cephei 4.15 4.21 0.06 0.98 h F0IV
HD 40372 5.88 5.92 0.04 1.466 h A5me In eclipsing binary system
α Lyrae (Vega) −0.02 0.07 0.03 2.57 h A0Va 5th brightest star in the night sky
HR 1170 5.77 5.91 0.14 2.39 h A9IV
δ Scuti 4.60 4.79 0.19 4.65 h F2 IIIp prototype
V701 Coronae Australis Lampens & Rufuen (1990) 5.69 5.73 0.04 3.25 h F2 III/IV
QQ Telescopii Kurtz (1982) 6.53 (blue) 6.58 (blue) 0.05 1.52 h F2 IV

Other examples include - σ Octantis and β Cassiopeiae

References

[edit]
  1. ^ "Light Curve". Hipparcos ESA. ESA. Retrieved 17 February 2022.
  2. ^ McNamara, D. H.; Madsen, J. B.; Barnes, J.; Ericksen, B. F. (2000). "The Distance to the Galactic Center". Publications of the Astronomical Society of the Pacific. 112 (768): 202. Bibcode:2000PASP..112..202M. doi:10.1086/316512.
  3. ^ McNamara, D. Harold; Clementini, Gisella; Marconi, Marcella (2007). "A δ Scuti Distance to the Large Magellanic Cloud". The Astronomical Journal. 133 (6): 2752–2763. arXiv:astro-ph/0702107. Bibcode:2007AJ....133.2752M. doi:10.1086/513717. S2CID 18053647.
  4. ^ a b c Majaess, D. J.; Turner, D. G.; Lane, D. J.; Henden, A. A.; Krajci, T. (2011). "Anchoring the Universal Distance Scale Via a Wesenheit Template". Journal of the American Association of Variable Star Observers (Jaavso). 39 (1): 122. arXiv:1007.2300. Bibcode:2011JAVSO..39..122M.
  5. ^ a b Majaess, Daniel J.; Turner, David G.; Lane, David J.; Krajci, Tom (2011). "Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars". Journal of the American Association of Variable Star Observers (Jaavso). 39 (2): 219. arXiv:1102.1705. Bibcode:2011JAVSO..39..219M.
  6. ^ a b Poleski, R.; Soszyński, I.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K. (2010). "The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. VI. Delta Scuti Stars in the Large Magellanic Cloud". Acta Astronomica. 60 (1): 1. arXiv:1004.0950. Bibcode:2010AcA....60....1P.
  7. ^ a b Cohen, Roger E.; Sarajedini, Ata (2012). "SX Phoenicis period-luminosity relations and the blue straggler connection". Monthly Notices of the Royal Astronomical Society. 419 (1): 342. Bibcode:2012MNRAS.419..342C. doi:10.1111/j.1365-2966.2011.19697.x.
  8. ^ Garg, A.; Cook, K. H.; Nikolaev, S.; Huber, M. E.; Rest, A.; Becker, A. C.; Challis, P.; Clocchiatti, A.; Miknaitis, G.; Minniti, D.; Morelli, L.; Olsen, K.; Prieto, J. L.; Suntzeff, N. B.; Welch, D. L.; Wood-Vasey, W. M. (2010). "High-amplitude δ-Scutis in the Large Magellanic Cloud". The Astronomical Journal. 140 (2): 328. arXiv:1004.0955. Bibcode:2010AJ....140..328G. doi:10.1088/0004-6256/140/2/328. hdl:1969.1/181688. S2CID 118386274.
  9. ^ I.A., Vasil'yev; et al. (1989-03-17). "On the Variability of Vega". Commission 27 of the I.A.U. Retrieved 2007-10-30.
  10. ^ a b (apparent visual magnitude

Further reading

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