Theory and Observation of Active B-type Stars
Active B-type stars are defined by their characteristic emission formed in a dense environment. Among them are the classical Be stars, which are surrounded by ionized gaseous disks, and B[e] stars, whose disks are so dense that even molecules and dust can form within them. The variability of active...
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| Format: | Electronic Book Chapter |
| Language: | English |
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MDPI - Multidisciplinary Digital Publishing Institute
2023
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| 100 | 1 | |a Cidale, Lydia Sonia |4 edt | |
| 700 | 1 | |a Kraus, Michaela |4 edt | |
| 700 | 1 | |a Arias, María Laura |4 edt | |
| 700 | 1 | |a Cidale, Lydia Sonia |4 oth | |
| 700 | 1 | |a Kraus, Michaela |4 oth | |
| 700 | 1 | |a Arias, María Laura |4 oth | |
| 245 | 1 | 0 | |a Theory and Observation of Active B-type Stars |
| 260 | |a Basel |b MDPI - Multidisciplinary Digital Publishing Institute |c 2023 | ||
| 300 | |a 1 electronic resource (390 p.) | ||
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| 506 | 0 | |a Open Access |2 star |f Unrestricted online access | |
| 520 | |a Active B-type stars are defined by their characteristic emission formed in a dense environment. Among them are the classical Be stars, which are surrounded by ionized gaseous disks, and B[e] stars, whose disks are so dense that even molecules and dust can form within them. The variability of active B-type stars seen on various time and spatial scales is often connected to the formation and dissipation of these disks. Although the possible roles of radiation, rotation, pulsation, and binarity in pulling material off the stars have been explored in detail in the past few decades, the relevant physical processes involved in the formation of sustainable disks and their dynamical evolution are still unclear and a matter of debate.This Special Issue intends to provide a comprehensive update on the state of knowledge in the field of active B-type stars. It combines reviews and selected contributions on recent groundbreaking advancements in the comprehension of these peculiar objects from both a theoretical and an observational perspective. These new insights form the basis for exploring complex physical phenomena to verify the different scenarios proposed for the evolution and variability of stars and their circumstellar environment of the diverse classes of active B-type stars. | ||
| 540 | |a Creative Commons |f https://creativecommons.org/licenses/by/4.0/ |2 cc |4 https://creativecommons.org/licenses/by/4.0/ | ||
| 546 | |a English | ||
| 650 | 7 | |a Research & information: general |2 bicssc | |
| 650 | 7 | |a Physics |2 bicssc | |
| 650 | 7 | |a Astronomy, space & time |2 bicssc | |
| 653 | |a stars: individual: α Eri, α Col, ω Car, η Cen | ||
| 653 | |a archive | ||
| 653 | |a stars: emission-line, Be | ||
| 653 | |a stars: early-type | ||
| 653 | |a (stars:) circumstellar matter | ||
| 653 | |a stars: peculiar (except chemically peculiar) | ||
| 653 | |a Be stars | ||
| 653 | |a early-type emission stars | ||
| 653 | |a circumstellar disks | ||
| 653 | |a early-type variable stars | ||
| 653 | |a open star clusters | ||
| 653 | |a Gaia | ||
| 653 | |a Techniques: spectrophotometric | ||
| 653 | |a Stars: activity | ||
| 653 | |a Stars: emission-line, B, Bn, Be, B[e], Bm | ||
| 653 | |a Stars: rotation | ||
| 653 | |a Stars: evolution | ||
| 653 | |a Stars: chemically peculiar | ||
| 653 | |a Stars: magnetic field | ||
| 653 | |a stars flares | ||
| 653 | |a stars activity | ||
| 653 | |a stars binaries spectroscopic | ||
| 653 | |a early-type stars | ||
| 653 | |a stars individual | ||
| 653 | |a HD 36030 | ||
| 653 | |a circumstellar matter: jets and outflows | ||
| 653 | |a stars: individual Z CMa | ||
| 653 | |a stars: emission-line | ||
| 653 | |a Be | ||
| 653 | |a stars: massive | ||
| 653 | |a stars: mass-loss | ||
| 653 | |a hydrodynamics | ||
| 653 | |a analytical methods | ||
| 653 | |a numerical methods | ||
| 653 | |a methods: statistical methods: numerical | ||
| 653 | |a binaries: eclipsing | ||
| 653 | |a stars: oscillations (including pulsations) | ||
| 653 | |a stars: peculiar | ||
| 653 | |a stars: individual: MWC 645 | ||
| 653 | |a circumstellar matter | ||
| 653 | |a binaries: general | ||
| 653 | |a techniques: spectroscopic | ||
| 653 | |a stars: supergiants | ||
| 653 | |a stars: winds | ||
| 653 | |a outflows | ||
| 653 | |a massive stars | ||
| 653 | |a mass-loss stars | ||
| 653 | |a star evolution | ||
| 653 | |a emission line | ||
| 653 | |a Be circumstellar matter | ||
| 653 | |a supergiant stars | ||
| 653 | |a star variables | ||
| 653 | |a S Doradus infrared | ||
| 653 | |a galaxies: individual | ||
| 653 | |a WLM | ||
| 653 | |a NGC 55 | ||
| 653 | |a NGC 247 | ||
| 653 | |a NGC 253 | ||
| 653 | |a NGC 300 | ||
| 653 | |a NGC 3109 | ||
| 653 | |a NGC 7793 | ||
| 653 | |a stars: symbiotic, binaries | ||
| 653 | |a stars: infrared | ||
| 653 | |a stars: individual: MX Pup, π Aqr | ||
| 856 | 4 | 0 | |a www.oapen.org |u https://mdpi.com/books/pdfview/book/8319 |7 0 |z DOAB: download the publication |
| 856 | 4 | 0 | |a www.oapen.org |u https://directory.doabooks.org/handle/20.500.12854/128849 |7 0 |z DOAB: description of the publication |