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With the understanding of the processes of emission line formation in the early 20th century it became clear that these lines in Be stars must come from circumstellar material ejected from the star helped by the rapid rotation of the star. All the observational characteristics of Be stars can now be
147:
Some Be stars exhibit spectral features that are interpreted as a detached "shell" of gas surrounding the star, or more accurately a disc or ring. These shell features are thought to be caused when the disc of gas that is present around many Be stars is aligned edge on to us so that it creates very
133:
explained with a gaseous disk that is formed of material ejected from the star. The infrared excess and the polarization result from the scattering of stellar light in the disk, while the line emission is formed by re-processing stellar ultraviolet light in the gaseous disc.
120:, the first star ever observed with emission lines. Many other bright stars were found to show similar spectra, although many of these are no longer considered to be classical Be stars. The brightest is
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when a transient or variable disk is observed. Be stars that show variability without clear indication of the mechanism are listed simply as BE in the
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lines in emission. These are sometimes referred to as classical Be stars. The emission lines may be present only at certain times.
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Although the Be type spectrum is most strongly produced in class B stars, it is also detected in O and A
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81:. It is preferred to restrict usage of the term Be star to non-supergiant stars showing one or more
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301:"Schreiben des Herrn Prof.Secchi, Dir. Der Sternwarte des Collegio Romano, an den Herausgeber"
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Be stars are often visually and spectroscopically variable. Be stars can be classified as
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Rivinius, Thomas; Carciofi, Alex C.; Martayan, Christophe (2013). "Classical Be stars".
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Struve, Otto (1931). "On the Origin of Bright Lines in
Spectra of Stars of Class B".
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Many stars have B-type spectra and show hydrogen emission lines, including many
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174:. Some of these are thought to be pulsating stars and are sometimes called
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and emission lines. A narrower definition, sometimes referred to as
422:"The influence of rotation and stellar winds upon the Be phenomenon"
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381:"Evidence for mass loss at moderate to high velocity in Be stars"
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B star whose spectrum has, or had at some time, one or more
124:, although it was not recognised as a Be star until 1976.
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338:
Merrill, P. W.; Humason, M. L.; Burwell, C. G. (1925).
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340:"Discovery and Observations of Stars of Class Be"
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499:Slettebak, A. (1976). Slettebak, Arne (ed.).
8:
112:The first star recognized as a Be star was
804:
579:
565:
557:
194:Porter, John M.; Rivinius, Thomas (2003).
445:
404:
363:
251:
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148:narrow absorption lines in the spectrum.
379:Snow, T. P.; Marlborough, J. M. (1976).
41:are a heterogeneous set of stars with B
186:
240:The Astronomy and Astrophysics Review
7:
426:Astronomical Society of the Pacific
172:General Catalogue of Variable Stars
14:
546:"Be Star Spectra (BeSS) Database"
2068:
2058:
2057:
1:
1970:Timeline of stellar astronomy
534:Hot and Active Stars Research
61:Definition and classification
538:Article from Olivier Thizy:
1630:Hertzsprung–Russell diagram
168:Gamma Cassiopeiae variables
16:In astronomy, a B-type star
2122:
1544:Kelvin–Helmholtz mechanism
532:Philippe Stee's homepage:
158:Gamma Cassiopeiae variable
155:
140:
18:
2053:
807:
594:
509:10.1007/978-94-010-1498-4
305:Astronomische Nachrichten
270:10.1007/s00159-013-0069-0
1923:With multiple exoplanets
325:10.1002/asna.18670680405
176:Lambda Eridani variables
19:Not to be confused with
709:Asymptotic giant branch
262:2013A&ARv..21...69R
162:Lambda Eridani variable
96:stars, but a number of
34:, the brightest Be star
2045:Tidal disruption event
1534:Circumstellar envelope
768:Luminous blue variable
35:
1570:Effective temperature
463:Astrophysical Journal
385:Astrophysical Journal
344:Astrophysical Journal
55:Balmer emission lines
29:
2040:Planet-hosting stars
1918:With resolved images
1889:Historical brightest
1819:Photometric-standard
1745:Solar radio emission
1539:Eddington luminosity
1319:Triple-alpha process
1257:Thorne–Żytkow object
632:Young stellar object
196:"Classical Be Stars"
73:, mass-transferring
1864:Highest temperature
1635:Color–color diagram
1500:Protoplanetary disk
1304:Proton–proton chain
982:Chemically peculiar
475:1931ApJ....73...94S
438:1975PASP...87..777M
397:1976ApJ...203L..87S
356:1925ApJ....61..389M
317:1866AN.....68...63S
299:Secchi, A. (1867).
212:2003PASP..115.1153P
116:, observed 1866 by
104:are also included.
1869:Lowest temperature
1620:Photometric system
1590:Absolute magnitude
1524:Circumstellar dust
1137:Stellar black hole
773:Stellar population
659:Herbig–Haro object
501:Be and Shell Stars
420:Massa, D. (1975).
71:Herbig Ae/Be stars
47:classical Be stars
36:
2083:
2082:
1986:Substellar object
1965:Planetary nebulae
1384:Luminous red nova
1294:Deuterium burning
1280:
1279:
763:Instability strip
743:Wolf-Rayet nebula
697:Horizontal branch
642:Pre-main-sequence
518:978-94-010-1498-4
114:Gamma Cassiopeiae
2113:
2075:Stars portal
2073:
2072:
2061:
2060:
1717:Planetary system
1640:Strömgren sphere
1512:Asteroseismology
1233:Black hole star
805:
731:Planetary nebula
692:Red-giant branch
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2106:1866 in science
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1974:
1943:Milky Way novae
1879:Smallest volume
1823:
1804:Radial velocity
1727:
1721:
1673:Common envelope
1649:
1548:
1517:Helioseismology
1488:Bipolar outflow
1429:Microturbulence
1424:Convection zone
1405:
1299:Lithium burning
1286:Nucleosynthesis
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622:Molecular cloud
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550:basebe.obspm.fr
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493:Further reading
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156:Main articles:
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1874:Largest volume
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1585:Magnetic field
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1495:Accretion disk
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1471:Alfvén surface
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1466:Stellar corona
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527:External links
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141:Main article:
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75:binary systems
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43:spectral types
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2035:Intergalactic
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2015:Galactic year
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990:
988:
985:
984:
983:
980:
978:
975:
971:
968:
966:
963:
961:
958:
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956:
953:
949:
946:
945:
944:
941:
937:
934:
932:
929:
927:
924:
923:
922:
919:
917:
914:
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868:
865:
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856:
853:
851:
848:
846:
843:
841:
838:
836:
833:
831:
828:
826:
823:
822:
820:
818:
815:
813:
810:
809:
806:
803:
801:
797:
789:
786:
784:
783:Superluminous
781:
780:
779:
776:
774:
771:
769:
766:
764:
761:
759:
756:
754:
751:
749:
746:
744:
741:
737:
734:
733:
732:
729:
727:
724:
720:
717:
715:
712:
711:
710:
707:
703:
700:
699:
698:
695:
693:
690:
688:
687:Main sequence
685:
684:
682:
680:
676:
670:
667:
665:
664:Hayashi track
662:
660:
657:
653:
650:
648:
645:
643:
640:
638:
635:
634:
633:
630:
628:
625:
623:
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618:
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614:
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589:
582:
577:
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568:
563:
562:
559:
551:
547:
543:
541:
537:
535:
531:
530:
526:
520:
514:
510:
506:
502:
497:
496:
492:
484:
480:
476:
472:
468:
464:
457:
454:
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431:
427:
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416:
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402:
398:
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382:
375:
372:
366:
361:
357:
353:
349:
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334:
331:
326:
322:
318:
314:
310:
306:
302:
295:
292:
287:
283:
279:
275:
271:
267:
263:
259:
254:
249:
245:
241:
234:
232:
228:
222:
217:
213:
209:
206:(812): 1153.
205:
201:
197:
190:
187:
181:
179:
177:
173:
169:
163:
159:
151:
149:
144:
136:
134:
127:
125:
123:
119:
118:Angelo Secchi
115:
107:
105:
103:
99:
95:
94:main sequence
91:
86:
84:
83:Balmer series
80:
76:
72:
68:
60:
58:
56:
52:
48:
44:
40:
33:
30:Depiction of
28:
22:
1938:White dwarfs
1928:Brown dwarfs
1911:Most distant
1859:Most massive
1837:Proper names
1797:Photographic
1750:Solar System
1728:observations
1655:Star systems
1478:Stellar wind
1461:Chromosphere
1434:Oscillations
1314:Helium flash
1164:Hypothetical
1142:X-ray binary
1081:Compact star
1033:
916:Bright giant
669:Henyey track
647:Herbig Ae/Be
549:
500:
466:
462:
456:
429:
425:
415:
388:
384:
374:
347:
343:
333:
311:(4): 63–64.
308:
304:
294:
243:
239:
203:
199:
189:
165:
146:
131:
111:
87:
64:
46:
38:
37:
1991:Brown dwarf
1767:Circumpolar
1645:Kraft break
1625:Color index
1600:Metallicity
1560:Designation
1529:Cosmic dust
1451:Photosphere
1217:Dark-energy
1192:Electroweak
1177:Black dwarf
1108:Radio-quiet
1091:White dwarf
977:White dwarf
627:Bok globule
152:Variability
137:Shell stars
102:giant stars
90:shell stars
67:supergiants
49:, is a non-
2096:Star types
2090:Categories
1953:Candidates
1948:Supernovae
1933:Red dwarfs
1792:Extinction
1580:Kinematics
1575:Luminosity
1553:Properties
1446:Atmosphere
1344:Si burning
1334:Ne burning
1272:White hole
1245:Quasi-star
1172:Blue dwarf
1027:Technetium
943:Hypergiant
921:Supergiant
182:References
143:Shell star
51:supergiant
1884:Brightest
1782:Magnitude
1762:Pole star
1683:Symbiotic
1678:Eclipsing
1610:Starlight
1411:Structure
1401:Supernova
1394:Micronova
1389:Recurrent
1374:Symbiotic
1359:p-process
1354:r-process
1349:s-process
1339:O burning
1329:C burning
1309:CNO cycle
1252:Gravastar
788:Hypernova
778:Supernova
753:Dredge-up
726:Blue loop
719:super-AGB
702:Red clump
679:Evolution
637:Protostar
617:Accretion
609:Formation
286:118652497
278:0935-4956
253:1310.3962
246:(1): 69.
108:Discovery
98:subgiants
2101:Be stars
2063:Category
1958:Remnants
1854:Extremes
1814:Parallax
1787:Apparent
1777:Asterism
1755:Sunlight
1705:Globular
1690:Multiple
1615:Variable
1605:Rotation
1565:Dynamics
1456:Starspot
1130:Magnetar
1073:Remnants
889:Subgiant
862:Subdwarf
714:post-AGB
540:Be Stars
122:Achernar
39:Be stars
32:Achernar
2030:Gravity
1979:Related
1899:Nearest
1847:Chinese
1695:Cluster
1668:Contact
1505:Proplyd
1379:Remnant
1267:Blitzar
1241:Hawking
1197:Strange
1147:Burster
1103:Neutron
1056:Extreme
1007:He-weak
652:T Tauri
471:Bibcode
434:Bibcode
432:: 777.
393:Bibcode
391:: L87.
352:Bibcode
350:: 389.
313:Bibcode
258:Bibcode
208:Bibcode
79:B stars
2020:Galaxy
2008:Planet
1996:Desert
1904:bright
1842:Arabic
1663:Binary
1483:Bubble
1207:Planck
1182:Exotic
1118:Binary
1113:Pulsar
1051:Helium
1012:Barium
955:Carbon
948:Yellow
936:Yellow
909:Yellow
748:PG1159
515:
469:: 94.
284:
276:
77:, and
21:B star
2025:Guest
1829:Lists
1710:Super
1364:Fusor
1237:Black
1222:Quark
1202:Preon
1187:Boson
1123:X-ray
1039:Shell
992:Ap/Bp
894:Giant
812:Early
758:OH/IR
588:Stars
282:S2CID
248:arXiv
128:Model
1700:Open
1595:Mass
1419:Core
1369:Nova
1262:Iron
1212:Dark
1022:Lead
1002:HgMn
997:CEMP
926:Blue
899:Blue
817:Late
599:List
513:ISBN
274:ISSN
160:and
100:and
2001:Sub
1735:Sun
1154:SGR
931:Red
904:Red
505:doi
479:doi
442:doi
401:doi
389:203
360:doi
321:doi
266:doi
216:doi
204:115
2092::
1034:Be
987:Am
970:CH
965:CN
884:OB
879:WR
548:.
511:.
503:.
477:.
467:73
465:.
440:.
430:87
428:.
424:.
399:.
387:.
383:.
358:.
348:61
346:.
342:.
319:.
309:68
307:.
303:.
280:.
272:.
264:.
256:.
244:21
242:.
230:^
214:.
202:.
198:.
178:.
69:,
57:.
1227:Q
1046:B
960:S
872:B
867:O
855:M
850:K
845:G
840:F
835:A
830:B
825:O
580:e
573:t
566:v
552:.
521:.
507::
485:.
481::
473::
450:.
444::
436::
409:.
403::
395::
368:.
362::
354::
327:.
323::
315::
288:.
268::
260::
250::
224:.
218::
210::
23:.
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