View source for Delta Scuti variable

{{Short description|Subclass of 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>]]
A '''Delta Scuti variable''' (sometimes termed '''dwarf cepheid''' when the V-band amplitude is larger than 0.3 mag.) is a class of [[pulsating star]], comprising several sub-classes of object with A- or F-type spectra.

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> and, together with [[classical cepheids]], are important [[standard candles]]. They 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 [[OGLE]] and [[MACHO]] surveys have detected nearly 3,000 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 of Delta Scuti variables 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.  They are usually A0 to F5 [[stellar classification|type]] [[giant star|giant]], [[subgiant]], or [[main sequence]] stars. The high-amplitude Delta Scuti variables are also called '''AI Velorum stars''', after the prototype [[AI Velorum]].  [[SX Phoenicis variables]] are generally considered to be a subclass of Delta Scuti variables that contain [[Population II]] stars, often [[blue straggler]]s, 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, stars that are more luminous than main sequence stars of the same temperature,  still contracting towards the main sequence.

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,<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==
{{dynamic list}}
{| class="wikitable sortable" style="font-size:90%;"
|- bgcolor="#efefef"
! width="15%"|'''Designation (name)'''
! width="15%"|'''Discovery'''
! width="8%"|''Maximum''<ref name="ReferenceA">''(apparent visual magnitude''</ref> ([[Apparent magnitude|magnitude]])
! width="8%"|''Minimum''<ref name="ReferenceA"/> ([[Apparent magnitude|magnitude]])
! width="8%"|''Range of magnitude''
! width="11%"|'''Period'''
! width="15%"|'''Spectral type'''
! width="25%"|'''Comment'''
|---
| [[γ Boötis]]
| 
| style="text-align:right; padding-right: 1em;" | {{ntsh|3.02}}3.02
| style="text-align:right; padding-right: 1em;" | {{ntsh|3.07}}3.07
| style="text-align:right; padding-right: 1em;" | {{nts|0.05}}
| style="text-align:right; padding-right: 1em;" | {{nts|6.96}}&nbsp;h
|bgcolor="{{Color temperature|7800|hexval}}"| A7III
| 
|---
| [[ε Cephei]]
| 
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.15}}4.15
| style="text-align:right; padding-right: 1em;" | {{ntsh|4.21}}4.21
| style="text-align:right; padding-right: 1em;" | {{nts|0.06}}
| style="text-align:right; padding-right: 1em;" | {{nts|0.98}}&nbsp;h
|bgcolor="{{Color temperature|7514|hexval}}"| F0IV
| 
|---
| [[HD 40372]]
| 
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.88}}5.88
| style="text-align:right; padding-right: 1em;" | {{ntsh|5.92 }}5.92 
| style="text-align:right; padding-right: 1em;" | {{nts|0.04}}
| style="text-align:right; padding-right: 1em;" | {{nts|1.466}}&nbsp;h
|bgcolor="{{Color temperature|7706|hexval}}"| A5me
| 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
|---
| [[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 - [[σ Octantis]] and [[β Cassiopeiae]]

==References==
{{Reflist}}

==Further reading==
*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.aavso.org/vsots_delsct AAVSO: Delta Scuti and the Delta Scuti variables]

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

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