{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,9,5]],"date-time":"2026-09-05T05:46:20Z","timestamp":1788587180771,"version":"build-2803163510"},"reference-count":18,"publisher":"MDPI AG","issue":"6","license":[{"start":{"date-parts":[[2015,6,2]],"date-time":"2015-06-02T00:00:00Z","timestamp":1433203200000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0\/"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Entropy"],"abstract":"<jats:p>The entropy production (inside the volume bounded by a photosphere) of  main-sequence stars, subgiants, giants, and supergiants is calculated based on B\u2013V photometry data. A non-linear inverse relationship of thermodynamic fluxes and forces as well as an almost constant specific (per volume) entropy production of main-sequence stars (for 95% of stars, this quantity lies within 0.5 to 2.2 of the corresponding solar magnitude) is found. The obtained results are discussed from the perspective of known extreme principles related to entropy production.<\/jats:p>","DOI":"10.3390\/e17063645","type":"journal-article","created":{"date-parts":[[2015,6,2]],"date-time":"2015-06-02T11:38:36Z","timestamp":1433245116000},"page":"3645-3655","update-policy":"https:\/\/doi.org\/10.3390\/mdpi_crossmark_policy","source":"Crossref","is-referenced-by-count":3,"title":["Entropy Production of Stars"],"prefix":"10.3390","volume":"17","author":[{"ORCID":"https:\/\/orcid.org\/0000-0001-7066-8768","authenticated-orcid":false,"given":"Leonid","family":"Martyushev","sequence":"first","affiliation":[{"name":"Department of Technical Physics, Ural Federal University, Mira St. 19, 620002 Ekaterinburg, Russia"},{"name":"Institute of Industrial Ecology, S Kovalevskoi St. 20a, 620219 Ekaterinburg, Russia"}],"role":[{"vocabulary":"crossref","role":"author"}]},{"given":"Sergey","family":"Zubarev","sequence":"additional","affiliation":[{"name":"Department of Technical Physics, Ural Federal University, Mira St. 19, 620002 Ekaterinburg, Russia"}],"role":[{"vocabulary":"crossref","role":"author"}]}],"member":"1968","published-online":{"date-parts":[[2015,6,2]]},"reference":[{"key":"ref_1","unstructured":"Prigogine, I., and Nicolis, G. 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Astronomy: Principles and Practice, IOP Press.","DOI":"10.1201\/9781420057034"},{"key":"ref_13","unstructured":"Available online: http:\/\/webda.physics.muni.cz."},{"key":"ref_14","unstructured":"Available online: http:\/\/groups.dfa.unipd.it\/ESPG\/."},{"key":"ref_15","unstructured":"Available online: http:\/\/www.fisica.hol.es\/."},{"key":"ref_16","doi-asserted-by":"crossref","first-page":"815","DOI":"10.1051\/0004-6361:20079165","article-title":"Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-AGB end for 0.15-2.5 Mo stars","volume":"484","author":"Bertelli","year":"2008","journal-title":"Astron. Astrophys."},{"key":"ref_17","doi-asserted-by":"crossref","first-page":"355","DOI":"10.1051\/0004-6361\/200912093","article-title":"Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 M\u0298 stars","volume":"508","author":"Bertelli","year":"2009","journal-title":"Astron. 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