Delta Scuti variable

From Wikipedia, the free encyclopedia
  (Redirected from Dwarf Cepheids)
Jump to: navigation, search

A Delta Scuti variable (sometimes termed dwarf cepheid) is a variable star which exhibits variations in its luminosity due to both radial and non-radial pulsations of the star's surface. The variables 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.[1][2][3][4] The variables follow a period-luminosity relation in certain passbands like other standard candles such as Cepheids.[3][4][5][6] 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.[3][6] The recently discovered Rapidly oscillating Ap stars are also a subclass of Delta Scuti variables, found on the main sequence.[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.[5][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. They are the second most abundant variable source in the Milky Way after white dwarfs.

δ – 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.

The prototype of these sorts of variable stars is Delta Scuti, 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 β Cassiopeiae. Vega (α Lyrae) is a suspected Delta Scuti variable,[citation needed] but this remains unconfirmed.

List of notable member stars[edit]

Designation (name) Constellation Discovery Apparent magnitude (Maximum)[9] Apparent magnitude (Minimum)[10] Range of magnitude Period Spectral type Comment
Gamma Boötis Boötes !B9988947431686 3m.02 !B9988783224384 3m.07 !D0029957322735 0.05 !B9980598205256 6.96 h A7III
Epsilon Cephei Cepheus !B9985768916657 4m.15 !B9985625373523 4m.21 !D0028134107167 0.06 !D0000202027073 0.98 h F0IV
Delta Scuti Scutum !B9984739436965 4m.6 !B9984334695885 4m.79 !D0016607312068 0.19 !B9984631327804 4.65 h F2 IIIp prototype

References[edit]

  1. ^ McNamara, D. H.; Madsen, J. B.; Barnes, J.; Ericksen, B. F. (2000). The Distance to the Galactic Center, PASP
  2. ^ McNamara, D. Harold; Clementini, Gisella; Marconi, Marcella (2007). The Distance to the Galactic Center, AJ
  3. ^ 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, JAAVSO
  4. ^ a b Majaess, D. J.; Turner, D. G.; Lane, D. J.; Krajci, T. (2011). Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting Delta Scuti Stars, JAAVSO
  5. ^ a b Poleski, R.; Soszyñski, I.; Udalski, A.; Szymañski, M. K.; Kubiak, M.; Pietrzyñski, 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
  6. ^ a b Cohen, Roger E.; Sarajedini, Ata (2012). SX Phoenicis period-luminosity relations and the blue straggler connection, MNRAS
  7. ^ Kopacki, G.; Kołaczkowski, Z.; Pigulski, A. (2003). Variable stars in the globular cluster M 13, Acta Astronomica
  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, AJ
  9. ^ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))
  10. ^ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))