Period-luminosity relation

Period-Luminosity relation for Classical Cepheid variables.[1]

In astronomy, a period-luminosity relation is a relationship linking the luminosity of pulsating variable stars with their pulsation period. The best-known relation is the direct proportionality law holding for Classical Cepheid variables, sometimes called the Leavitt Law.[2][3][4] Discovered in 1908 by Henrietta Swan Leavitt, the relation established Cepheids as foundational indicators of cosmic benchmarks for scaling galactic and extragalactic distances.[5][6][7][8][9][10] The physical model explaining the Leavitt's law for classical cepheids is called kappa mechanism.

  1. ^ Storm, J.; Gieren, W.; Fouqué, P.; Barnes, T. G.; Pietrzyński, G.; Nardetto, N.; Weber, M.; Granzer, T.; Strassmeier, K. G. (October 2011). "Calibrating the Cepheid period-luminosity relation from the infrared surface brightness technique: I. The p-factor, the Milky Way relations, and a universal K-band relation". Astronomy & Astrophysics. 534. EDP Sciences: A94. arXiv:1109.2017. Bibcode:2011A&A...534A..94S. doi:10.1051/0004-6361/201117155. S2CID 96456751.
  2. ^ Johnson, Kirk (March 27, 2024). "Overlooked No More: Henrietta Leavitt, Who Unraveled Mysteries of the Stars - The portrait that emerged from her discovery, called Leavitt's Law, showed that the universe was hundreds of times bigger than astronomers had imagined". The New York Times. Archived from the original on March 27, 2024. Retrieved March 28, 2024.
  3. ^ "A century of cepheids: Two astronomers, a hundred years apart, use stars to measure the Universe" (Press release). Sloan Digital Sky Survey. 9 January 2018. Retrieved 23 September 2019.
  4. ^ "Society Resolutions". American Astronomical Society. 8 March 2021. Archived from the original on 8 March 2021.
  5. ^ Udalski, A.; Soszynski, I.; Szymanski, M.; Kubiak, M.; Pietrzynski, G.; Wozniak, P.; Zebrun, K. (1999). "The Optical Gravitational Lensing Experiment. Cepheids in the Magellanic Clouds. IV. Catalog of Cepheids from the Large Magellanic Cloud". Acta Astronomica. 49: 223–317. arXiv:astro-ph/9908317. Bibcode:1999AcA....49..223U.
  6. ^ Soszynski, I.; Poleski, R.; Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Wyrzykowski, L.; Szewczyk, O.; Ulaczyk, K. (2008). "The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. I. Classical Cepheids in the Large Magellanic Cloud". Acta Astronomica. 58: 163. arXiv:0808.2210. Bibcode:2008AcA....58..163S.
  7. ^ Freedman, Wendy L.; Madore, Barry F.; Gibson, Brad K.; Ferrarese, Laura; Kelson, Daniel D.; Sakai, Shoko; Mould, Jeremy R.; Kennicutt, Jr., Robert C.; Ford, Holland C.; Graham, John A.; Huchra, John P.; Hughes, Shaun M. G.; Illingworth, Garth D.; Macri, Lucas M.; Stetson, Peter B. (2001). "Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant". The Astrophysical Journal. 553 (1): 47–72. arXiv:astro-ph/0012376. Bibcode:2001ApJ...553...47F. doi:10.1086/320638. S2CID 119097691.
  8. ^ Tammann, G. A.; Sandage, A.; Reindl, B. (2008). "The expansion field: the value of H 0". The Astronomy and Astrophysics Review. 15 (4): 289–331. arXiv:0806.3018. Bibcode:2008A&ARv..15..289T. doi:10.1007/s00159-008-0012-y. S2CID 18463474.
  9. ^ Majaess, D. J.; Turner, D. G.; Lane, D. J. (2009). "Characteristics of the Galaxy according to Cepheids". Monthly Notices of the Royal Astronomical Society. 398 (1): 263–270. arXiv:0903.4206. Bibcode:2009MNRAS.398..263M. doi:10.1111/j.1365-2966.2009.15096.x. S2CID 14316644.
  10. ^ Freedman, Wendy L.; Madore, Barry F. (2010). "The Hubble Constant". Annual Review of Astronomy and Astrophysics. 48: 673–710. arXiv:1004.1856. Bibcode:2010ARA&A..48..673F. doi:10.1146/annurev-astro-082708-101829. S2CID 119263173.