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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. The variables follow a period-luminosity relation in certain passbands like other standard candles such as Cepheids. 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. 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. 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, but this remains unconfirmed.

Examples

Other examples include - σ Octantis and β Cassiopeiae

References

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. ^ 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. ^ 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. ^ 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. ^ 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. ^ (apparent visual magnitude

Further reading

• Samus N.N., Durlevich O.V., et al. Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)
• AI Velorum star at The Encyclopedia of Astrobiology, Astronomy, and Spaceflight
• AAVSO: Delta Scuti and the Delta Scuti variables

v t e Variable stars
Pulsating	Cepheids and cepheid-like Type I (Classical cepheids, Delta Scuti) Type II (BL Herculis, W Virginis, RV Tauri) RR Lyrae Rapidly oscillating Ap SX Phoenicis Blue-white with early spectra Alpha Cygni Beta Cephei Slowly pulsating B-type PV Telescopii Blue large-amplitude pulsator Long-period Mira Semiregular Slow irregular Other Gamma Doradus Solar-like oscillations White dwarf
Eruptive	Protostar and PMS Herbig Ae/Be Orion FU Orionis T Tauri Giants and supergiants Luminous blue variable R Coronae Borealis (DY Persei) Yellow hypergiant Eruptive binary Double periodic FS Canis Majoris RS Canum Venaticorum Other Flare Gamma Cassiopeiae Lambda Eridani Wolf–Rayet
Cataclysmic	AM Canum Venaticorum Dwarf nova Luminous red nova Nova Polar Intermediate Supernova Hypernova SW Sextantis Symbiotic Symbiotic nova Z Andromedae
Rotating	Non-spherical Rotating ellipsoidal Stellar spots BY Draconis FK Comae Berenices Magnetic fields α Canum Venaticorum Pulsar SX Arietis
Eclipsing	Algol Beta Lyrae Planetary transit W Ursae Majoris
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