© 2007: Instituto de Astronomía, UNAM - Circumstellar Media and Late Stages of Massive Stellar Evolution Ed. G. García-Segura & E. Ramirez-Ruiz masa Key with siv are b La estrella. wind donde es mass Los R ulae Nacional in tory Morelia, de (WR) forman siv de mass-loss particularly Mass photoionizing man the stellar sion, for quence, gian b initially massiv undergo 64 WIND-BLO y e evMexAA 1 e e the determinado una the masa ev greater Mass-loss The Cen stars used t y energy Wor estudios stars and m stars. difficult oluci´ and (RSG) with no terminal loss W y la e tro in ust progenitor medium estrella Mic burbujas curren Aut´ ds: v and b olf-Ra a terstellar stars se estrella to en En more HI ariables o elo dominate history on dominates de luminous hoac´ b ccurs a than cono onoma H illustrate input (Serie e las once w y este to shells de v O Although de Radioastronom , dominates inferred ery tly I radiation y an, is the 25 massiv 1. v de I W etapas et star las b cen p elo las . pierde o that REGIONS y WN art essen or the en olf-Ra azules M accepted v itself INTR de high M During in masa and (WR) de curren er surrounding estrellas cit winds ´ exico their ´ con blue nebulosas to ıculo,

la to el M the the star e y a Confer . of tially from ´ , exico, previas. circumstellar estrella mass-loss masa the out medio than longer RSG ODUCTION y The w BUBBLES m 40 the luminosas and (j.arth the et v the t ev and en differen e the ariable uc ´ and has ıa se mass-loss ev M to olution (WR) vironmen in m can studies ha encias) Ap most previous O y ev 25 a stellar — describ olutionary final to terstellar

uy main [email protected]). luminous distances left circunestelar timescale. de una ionizing Astrof do. olution progenitora M precisi´ Duran star median ev sup ST determine masiv t rate (LBV)

anillo star olv massiv the stages sup (LBV) tasa of ARS: P sequence , of erno on ´ ısica, winds. en ostal rate medium. t to ed 30 on, v te mass-loss but main erno as through to the ery te of the AND las photons and , m of blue Red v y stars. scenario stage la e est´ 64–71 in sup a and particularmen 3–72, uy sim Univ MASS v prop de some at v ring stars massiv diferen ery secuencia main for a misma, a directly the e sequence. circum- Indeed, alta erno and ulaciones v Sup lo dominada las stellar ersidad explo- in ariable of These orcionan Mas- 58090 w stars mas- their neb- (2007) HI terestelar. ev tens his- will S. can ABSTRA en- v for p cascarones er- RESUMEN se- WR LOSS e v tes olution a, ero elo J. , I stars, a of un ´ etapas REGIONS principal t cit Arth (LBV) a stages, w Studies n parsecs te ba o p um y algo hasta . or although of stages una ing strong stars through mediate circumstellar hanced, and siv cumstellar tral. sities bubble sonic H ulations, regions The gions CT ur ja The ´ Estas ericas. su I the de 1 en e v de I stars Massiv In 2. the elo on v of regions observ distancias p immediately stars y from F ez that in HI la stellar informaci´ compared ´ presup erdida EARL circumstellar this or are cidad. the stellar la the highly it dos and que these ev circumstellar episo their pro stars que the ho fase creates. e end the oluci´ is separated AR ring ed medium pap initial w fases are stars < Y la vide erno de wind shap mass dic ro medium P large winds regions the WR ionizing star. sup that 0 their er, estrella EV on or on de OUND v masa, nebulae dean . to 1 ery v mass est´ are some ed a lo ersonic circumstellar b OLUTION: acerca w p and mass del algunas loss the los ha n egin c In will medium en e liv an tan small throughout um b b b a for are v sho medium aunque REGIONS vironmen medio y y can orn this es vien sale e estimated the photon loss. rates m information to, separadas b and b of to phases a their ultracompact ers w, de uc as v e stellar MASSIVE W ( ery in tos b el lo article, decenas de the < dominated affect has e red la Th through olf-Ra of HI w-densit around are am circunestelar dense 0 las v la high EMBEDDED will estelares ionizing . historia luminosit suc ery us, progenitor 4 t en estrellas where shells sup bien their winds secuencia not p tasas is formation vironmen their h p y c b n the differen and molecular et ergian th or de umerical e small for on te a y kno n dense us liv , phase, that 40 umerical b the una de presup presup parsecs blo H de compact photons the hot, the en y hip y es. wn W determined . I ST M p ts, the ionized vironmen w I la t principal. star. star alrededar ´ erdida olf-Ra The ers´ surround t etapa resulting and regions). previous rate

dep sho bubbles exactly p of ARS the H the mo erno erno h ´ erdida clouds onicos star. yp de I mas- loses c neu- den- end- sim- I dels H and and k F cir- im- y er- re- de en ed v v or et la I a a t I , © 2007: Instituto de Astronomía, UNAM - Circumstellar Media and Late Stages of Massive Stellar Evolution Ed. G. García-Segura & E. Ramirez-Ruiz tions order the The and stellar spherical Within so without and bles latter b tions in ula the lik with H is This closer cometary Mac al. 30% vironmen gions nebulae et optical frequencies. b ionized lution. ing explained observ densit calculated means nism stars. & lifetimes then, inhibiting y o I ely an mo ok al. although Ch I 1994; turbulence As The (M20) off-cen H maternal collab regions, infrarred effect that of Lo is observ suggests inhomogeneous ving urc is 1979). represen of classical, y are I w to that ed to wind the that I ultracompact resp w w gradien ork sho nebulae The this high suc stellar region H h of Lumsden a a t repro shell in of form usually w orators (1992). of simply v and ter 3. their through I H of b wn c h massiv ell onsible elengths. I instabilities these ations sho the hampagne some y of a shell, suc including irregular Mo I extinction MAIN-SEQUENCE as regions Radio massiv molecular I sp ts in Mac b that around 1989; duce in the (Mellema the ws ts (Kurtz motion, b region spherical morphology h o the ving expansion, ectra ab b ecomes a w-sho Figure small, pro as only ear due (T w e that Lago b a ionizing More out stratified for & its ell-do Lo Orion the stars, y e enorio-T surv the those Kurtz duce c and star, medium, in Hoare little hampagne-t stars of Arth Sp w shap confining the to expands et the c 10% visible en it flo ha on in k photoionized y densit in cloud, confined observ eys 1, some ectacular et recen al. oung, compact cumen vironmen et ev H is w, v suggests mo c Nebula hot, or stellar mo these Nebula ur e es hampagne where the star in resem olution et for I al. imp of 1994; al. of 1999; I b agle ha whic densit b del, deled and & een this at regions. tly y WIND-BLO the w al. o suc the sho ed (1991); v up ultracompact and it 2006), wsho ionization ortan ted in ell-observ these star-forming e gradien Hoare , wind radio blance 1979; h the to it 1994). yp h b compared (M82), W lifetime ST H sho (M8) c radio n stage filamen Zh the t. to H images that y ecomes k is b of umerical as cases photo can alsh e I ed a c y A I distribution, t u I 10 k, wn H I kinematics gas H what flo an that flo roughly sim in GE T regions to although and v region Bo et wind (2006). They some ts, 5 I I sho enorio-T mo b an of ws morphology to w et I I the This include T ed e that H (Gaume ts ev yrs ulations al. is denheimer regions, of regions of WN fron their rifid pro visible al. seen with w dev dels or the Buren has infrarred I ap in expand- in sources. I massiv calcula- bubble. 2005). sim mec H regions ionized the can (W resem- blister ha region 1998). orates duced t stage, elops, detail hemi- up these BUBBLES I Neb- text- b w This that ev I it agle v also ula- and o een ha- the are en- ere e re- o b or or at to o- in et in & is d a e e shell at rounded up ble. idence in v sequence v ory Williams sho scale: trapp sw tect is 10 0 wind H ev while main 1999). gas a mo sequence or n len pla white. v The Fig. an dimensional AND . elo olume 0 2 > dynamic to olution. − I then v ept exp( t, 10 y I del w wind exp A 6 ery v cit p 30 predicts gra due regions 1. the a c) The clump ≤ 4 M expanding ed the is a sequence stellar y H up the z onen km rˆ the lo K, yscale of

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temp Mellema POST-MAIN-SEQUENCE F Dynamical b ries treatmen in yrs, rom ottom ha studies once around strong, stellar dynamic t erature a v 1972; slo e and mass r this wind-blo structure medium b wly − a axis). et & een 2 fiv star t of wind stars W al. figure ev densit fast, Mac is of in e loss ea the olution and carried differen to sho 2006). The lea this v wn bubble. and er Lo WR of the wn will is y ev it v radiation-h es et densit w bubble scenario gradien olution at initial can of on t it in Densit out the al. (1995a). wind o y uniform an terstellar is ccur z a b y 1977) A in slices p e H main b ositiv is masses to t seen y theory y I RSG expands. of I EV w within sho in ydro Garc and region this as through the ceases pressure e sequence. OLUTION the wn that medium. or linear dev temp dynamic ´ en ıa-Segura (e.g., 60 wind-blo on in immediate LBV vironmen the elop the to a M An erature a the scale turbulen Dyson

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short sho filamen their mass wind-blo y 1996b; wn o wn X-ra X-ra the not the the Arth R W tral to consisten of date, ha G2.4+1.4, drops. CW S wind hot main c erature and describ Anon(WR y WR the wn and OLF-RA bubbles, the k the et bubble v stellar X-ra 308, break main y enhanced WR y in around dynamical e loading ur star in 104, of an bubbles ts satellites sho is teraction shap emitting F densit cores. stars y S four The acceleration to ev filamen wind. wn and rey et comp dense y O6.5fp t are WR 308 inheren ha ap ed wind Ra c NGC with sw the as up, and emitting k al. to and material er ed v bubbles is YET of WR 128) ed sim orating clumps yleigh- o e ept-up photo- y this ab in around of rev it onen wind, 1993, et They these these c since (Gru- co RSG wind- RSG b star), ts 2359, there map har- WR The o ula- ion- and but age een gas the the and ex- 116 eal v tly re- ol- al. 67 of e. is t © 2007: Instituto de Astronomía, UNAM - Circumstellar Media and Late Stages of Massive Stellar Evolution Ed. G. García-Segura & E. Ramirez-Ruiz 1999; tiv and sp wind temp bles, detection temp Fig. 68 24,000 (Y.-H. dep temp in h fraction detection liv mass wind is elapsed w absorbing tion of S star and from Ch minosit ther ydrogen e terv 308 ectra ed, that ely the u sho Another ends the 4. the sim that ha erature eratures eratures namely parameters et exp is ening ASCA Ch ( (Bo w lasting, y In WR v ∼ y Ch the ears star ulation time in suggest e al. X-ra of teraction the u elled strongly of obtained 1 teracting (W not c u, of of H et hk the × the X-ra wind 2003). has T HI after v I y rigge that priv. in X-ra X-ra observ arev 10 p al. ariation of in b ≤ in column emission ossible sa emitted mo een describ column the an 34 y are a 1 10 the the 2003). y the . of with ys ys extinction , on 5 emitting p del 4 et erg 1988; ionizing comm.). for with tailored WR × ations, ossible a the only The K. RSG range from in onset al. the mass-loss 10 is of NGC densit s ed the − W explanation flux that is the 6 larger stage The 2005). total W 1 the parameters 20% olf-Ra ab column K phase v photon WR from of rigge 1–5 RSG explanation ery stage W to 6888 o and can y other F pla RSG softness the v the rigge or X-ra during e. and in of rate an × y sensitiv ys wind-blo and et XMM b 1 et shell X-ra The WR magnitude y 10 ( fitted is the . rate e densit ∼ 0 shell. an wind y wind-blo to particular of al. 6 absorb et × relativ sw luminosit 9 y the for K of imp wind. total M of the 10 × time of for ˙ e 1994; ept al. observ emitting with temp w for y suc 10 6 wn these the S b In in ortan amoun = the ∗ oth K, of the ely 34 ed 2005), up X-ra teraction h wn = the Figure the The 4 the bubbles than sim erature neutral erg W resp . a ations, b y 3 1 b ob 40 to short- X-ra t . y y rigge large × 86 bub- y non- with non- dense WR ula- M rˆ cen ject t s gas the the the ole ec- lu- 10 ei- − × or AR of

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Lozinsk The w Marston ized serv medium tiple v sho bubble pro remnan are frared emission, and through w cluded ermost cess of Our namic the 70 This as b shell b of co coming ap erno een oth ere e wband oling v the that cases the wn duce a It By Man In commen shaping orated the ations. expanding X-ra is innermost filamen t exterior mainly sim concen remnan mixing v m of argued to is In stellar order a or not cold ablation in and sup the thermal ts ust a of around shells RSG observ y at rate the in ulations y ys remnan h the ev a 1996; around images, increase 21 Figure a of W ydro hot, to b y erno around necessary flo few en end 1982). oth b t ts T shell of tric emitted progenitor olf-Ra the burst formed cm to ev circumstellar (Ch this t X-ra e or ws yp that could H that can ed a are, optically dynamic sho help v Cappa olutionary mixed slo the shells cases, I explain of e LBV of a conduction main through 6. t nebula shells radio I u 7. with for and b the y circumstellar sho wly ev I will c afterglo y ha region the y this 0.5 em FINAL the I nebular et k star indeed, et luminosities b to en during ed the v S and b w in e are stage represen star b sequence e al. y there stars (generally the w t et in – of expand. 308. densit edded WR unco wind additional WR due the b b diameters that a the and pro to (Marston 1 wind-blo hot y y v al. often the material, 2003; and T ws stage elengths k sho consists the the ST and yp the photoionized the imp cesses. presen eV, material v are in wind stage, amoun is to 2005). expansion bubble y prob er bubble the in A e clumps t c neutral previous evidence WR our visible k wind main-sequence medium GES and material ortan teraction thermal in W Ib/c although rev the X-ra surrounded , ed Just rep wn terstellar e v surrounded em rigge t mass-loading up 1996). exp eals t the calculations, the and observ stellar These of sim W wind orted structure (Chev to y bubble, b t or and sup from bubbles as e and to in edded shell. a for emitting < innermost ulation circumstellar the of enhance et ha stage, b in that for ejected ev erno optical eac 100 lo y b (Ch not 10 softness of able the in v alier structures y the ab filamen ap w-densit wind al. The the structure h e medium. h dynami- the b ydro photo a km v the u out oration clumps This p not the y as b a sup subse- 2005). it of so stage. reion- X-ra c at to 1981; y et RSG m dur- pro- nar- nar- out- WR gas, and and and soft s has to dy- ob- the the the 8% su- re- re- er- in- in- ul- ts. al. − AR of e- is y y o 1 THUR of siv teraction time. stand rev stabilities are stages circumstellar observ genitor b of circumstellar (dotted Arth ro no (Dopita tails and Bo to Arth Arth Bo n after a Fig. um oth 40 w v wind-blo structure c denheimer, e mo eal MNRAS, 313, 1979, a The hk created, b in 7. ur, ur, ur, sp stars of M a remnan at er arev, ving ternal a ed Ho imp total ectral are Radial

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