Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Lizano, S.; Galli, D.; Shu, F.; Cantó, J. Champagne Flows and Winds in H II Regions Revista Mexicana de Astronomía y Astrofísica, vol. 15, septiembre, 2003, pp. 166-171 Instituto de Astronomía Distrito Federal, México

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How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México 166 R Discutimos calen p en calen de lo exp en flujos W found self-gra la b molecular instan the this tributions a “on-the-sp Equation also c Key the initially 1939): ionized discuss no hampagne y or evMexAA w sho e tre v w 1 2 3 1 que presi´ the olv Recen F Instituto Osserv National Instituto onen “c discuss formation una Wor the densit pap ionized or tado tamien c la taneously de hampagne k en ha vit formation self-similar a the is on autogra ev te fron ds: er at te distribuci´ spherically atorio c tly (1) y giv hamp´ fuera sido olution y that ot” cloud n pro rest, w externa Tsing de de ev and la HI the to flo , (Serie t . cloud distribution, en e Z assumes olution Sh that expansi´ Astronom Astronom r ws. appro ducen Adem´ I iniciales di of will 0 llamada r 1. are v CHAMP an. expansion b thermal de S the REGIONS u at edad Hua Arcetri, y phase”. n cores a of of INTR on core e de the tra et equilibrio heated discuss n t solutions de massiv ximation. size symmetric as, a the p Univ un = on of de v Confer y ionization al. massiv α ´ ´ ıa, ıa, la standard els through o with la 2 ODUCTION la 0, discutimos p the Florence, pressure c r de curren densidad ersit 4 UNAM, UNAM, ho n S o The (2002; presi´ ρ e in out π of “fase w ub the part of A un r que strong erful to star ∝ — encias) y 2 e p mec´ an e GNE , for the dr expansion o of In n star Hsinc subsequen on the ionizada molecular r w a ST ucleo ´ this que form de of initially S. equilibrium − Italy Morelia, M mec er-la at the anico is = stellar hereafter t region t n the ´ exico como ´ ARS: ermica, cloud, = Lizano, stellar , their at self-similar. la h c N , its sho via hamp´ . u, ˙ hanical ab ula with 15 w 0, ∗ molecular FLO ev the . T expansion p o D.F., cen ja c , winds el aiw densit oluci´ M a v or ley that k (Str¨ results t self-gra of F 166–171 cloud e, accelerating ´ winds an”. exico. cen a tra 1 flujo 3 whose es ter. ORMA flo an. la SLGCL) WS / the n tra D. de M and balance omgren 2 on autosimilar. w v e ter. can formaci´ y ´ exico. in ´ es is v < core, Galli, p subsecuen La If inner (for Because autogra vitating, ´ es de and dis- of ABSTRA otencia the the the (1) de strength RESUMEN AND b n In (2003) the of TION de e expansi´ massiv los r este < 2 on region la initial  the F. fuertes 3. vitan of de n del c — static, te 100 Sh WINDS ub e Debido ho alen will The generally h electron com the core dius If Bondi-P ter toh order cloud is CT gas on the This una ydrogen, stars u, para e, at te que, an the radio, ST ionization A ydro de (p 3 star t bination to b vien steep acelerando singular U) square b ma t ARS: increasing and estrella Bondi-P e erhaps singular elo core core virial of > la inside sup r cuy al considerably dynamic) y ark caused (assumed tos densit  w 0 ρ regi´ magnitude appreciably empinado J. b densit ersonic a is N ∝ IN e whic is er b 100 MASS ˙ of de v Can in ∗ efore co on via inicialmen considered connected these and masiv elo r ark heated radius tensidad y the − is cloud efficien las , b h H el A function y n in cit t´ a y er n o the U, profile, all heating terna v supp to con gas 4 star p disk) sound y I estrellas a c the elo LOSS radius p I hampagne r r is smaller causado (thermal, of argumen en core b of erfil 2 1 larger out rate t REGIONS cities a e 3 ≡ ≡ the orting resulting te formation this to the / es to su a a v to to of 2 pressure elo sp de GM GM en constan c of t is the 2 2 of una of the haracterized < cen ion mak ha the a a gas eed > masiv than neutral in cidades densidad, than equilibrio appro 2 2 1 2 mec the p ionizing n ts ∗ ∗ v the tro. second 0 or outer what e turbulen densit , . flo funci´ exp e in < in esta yield hanical fallen im a ionized a ws. t) la as r is gradien 1 2 the 3. original ximated the Si onen 1 star , balance gas, and . falta on sup den has th denoted en y conectada la Este energy , original photons r los caracterizado H us, v in crecien t, α 0 t of ers´ b ionizaci´ tro elop r b I gas, to balance 2 n y de 0 ts I gradien or ∼ een the mass . onicas n is (neutral) is a gas to b the de pro ucleo ´ W e balance magne- r lev et p the the b equiv- 1 of called te e o o cloud y , w estos duce from a on w ccur el cen- M also a 2 2 een the the del (3) (2) tes a ra- er- re- b en es of la ∗ 1 is y y . , Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México If in can as flo gra a rium w tially (equation gular K “ionization ized ρ/ K lik F where 3 T output 2 regions when or b v K r r 1 b the 2 2 / . olume or eing e aking km ard, 6 to ∗ ∗ cr n , finite 2, 2 w ely K ' out K × “densit vitationally ionization the Assume One Since F µ : implied < M > ignore ph cr the ∗ the or of gas, i 10 s , 10 with m momen had − ionization w the ∗ if in 3 µ K ysical = K − ionized 1 the 2 H of ard, / the of of ' i radius can to , t it H cen cr 13 2, A cr . ypical  is m K a densit 4) ultra y 25 a the 25 gas U, , I has (3 a = cm the 2 the H I ∗ H ratio b the ter no but p compare this b b initially disk 2 M region tum), ounded” M ' 2 − radius I represen y o with ounded”. is µ 3 b surrounding I b µ w w ultra violet not gas

r i

gra ounded, s to n un ey mean the i region 10 y S the m er-la − b that n m , K ) of calculation that if , (and ounded 1 ond constan um b mak r H M vitational km , b H and ∗ will already ρ it 0 whereas ound violet can equations assumption K oth h ( ∗ = w " of extended ' b the radiation r has the ydrogen ts  w ∗ s (see (2 r ) the e ers, lo b − /K distribution empt (3 10 0  eigh the b the = ey a at r w n 1 . a In 4 (2 e part v ev 1 , and t H radiation 4 er − π The star cr ond − K alue rough molecular either cloud. Osterbro n w A and reac least K en t H M I r the m star. n y ' 4 r mass) 3) e I U, 0 − indicates 3 field p − π ) densit I − uc in (6) ∗ equals in mass, a in er gas ha I r of dividing 23 M n r of can 3) hed n α r w 0 N 0 α 2 h to sligh . w latter region that 2 ˙ initially 2 . v n ionization ∗ ' estimate particle mass ard (3 2 K 4 and ∗ Since ard of e − exterior SELF-SIMILAR . m Muc π the will stars is ionize ' 3 pressure cr y of − c r r uc t k and the N 25 1 0 a 3 cloud trapp of b the n from 10 with ˙ (5), amoun gas h N 1989). ounded that star case, ∗ M ) ' h critical is ˙ expand r line M / r 49 # are ∗ bigger 0 star 0 (2 ∗ n b 1 in of p 10 an said 

densit :  s / w of to has p efore ed r the n o 1 − terior 2 (or b , core b / 0 e the lik 4 w the − equilib- = a 1 ounded , t 2 infinite r et K r A on as within er , get If a 2 . of ely 2 3) arises fallen to v v finite more U w α 1 n , than , alue out- alue y w n ion- H and an 1 e 2 one la ini- een an- the the (4) (7) (5) (6) / b ell  to to > = ' ' w 2 I y e I . CHAMP Lizano, ized ties. densit ronmen with cen assumed in see the also serv der of Gara Bo T G con than resolution (e.g., with dicate & serv expansion scales the ionizing 1995; similar will side created mec V of regions regions After tablishes the pro from the with in ha enorio-T acca A 32.80+0.19B, v massiv the a denheimer, the Lizano tly tin duce Densit The When e GNE T hanical ations Gara densit ed cloud, most ionized then scales star b y gas 1 This p masses ak the a the , the y uum een Gara Lumsden roughly o et range initial & ∼ < manner F t w “c sho compact profiles with found & et purp b photons ranco y an is er-la e p Ro accelerating n al. FLO at outer dev y an hampagne passage agle, y start, y massiv K is o D’Alessio as infrared extensiv al. stars 2001). accelerating o c & to y p ∼ < sp w gradien the profiles k balance dr ccurs. , gas, expansion t 1996), ossibly kno M 3 elop isothermal ose w densit M er ∼ densit w 2. Lizano ectra ´ WS 2000; / propagating = Lizano, ıguez b T ard as ∗ et 2 & ∗ are exp y − regions densit la K enorio-T G within wn idealized esp & Theoretical e > 0 of < 2 accelerating implies w SLGCL, M H ∗ c of al. Bo , 61.48+0.09B1) O ely hampagne rapidly y 30 Note ected t and Hoare sev w y indicating the n ecially Ho < of this as I ∗ in clump Hatc exp 1990; 3 the and 1999; I phase” ell the denheimer gradien stars gradien (2000) 1999). < y M (as a eral K w ultracompact the studied massiv & regions w dense expression of the onen and distributions radio appro 3. ev

cr IF, pap agle, structure hell a inner that the of excitation . indicated G´ y Caselli , instan y 1996; er, the “c McKee for mo These if ma at sources the gas omez on the er from ts c a of ts mo ts hampagne ha et Ev hampagne-flo suc pressure and e ximated recom & flo if v that y constan the sho molecular whole in in regions is scales the observ es close v molecular with al. (e.g., to ionization dels cloud en taneous b ws 1990). w e Y h Lebr´ & to this e self-similar sev massiv c the ork the e to 1994; argued & gas sup on with k the stars 2000; expansion though densit as bination My ha b assume of discuss b 2 to eral tra H infinit T y e with on, cloud. of ationally inferred y the t remains range ersonic cen v G b ∼ follo an H gradien < the expand to 1979; ers I the e y n v v cen phase” I ten High T e 29.96 are Keto I for elo n els app cloud tral p Ro y I found regions 2002). = of righ sup cores that cores exp 1995; fron formation w ws. o ' regions y ∼ tral ths < results the b cit w a that 3. the (Osorio, through dr b the earance line F and ounded Due mo mo 3. ersonic er 10 spatial t-hand − onen review v of rate ts source orn ranco, y ´ t out ıguez, faster et of elo They radio cores (e.g., (e.g., en stars 0.02, ha ha 4 la (IF) self- V in dels dels ion- H will Re- 167 ob- ob- p N es- in- vi- ws ci- an al. K. v v to to ˙ in of of of of ts c, I e e ∗ I Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México assumed. the v where and the where it summarize stream) conditions side and and v sion tial and where 168 will sho ance and The it subsonic induce ariable elo y y   ( ( ( w v equation, v Neglecting F Substituting v v cities. gra equations reduced (9), w the b solutions consider : u of heating ollo ed these − b − y e − et ρ an the vit c x the the x define that wing hampagne reduced w x one ) is of ) flo 2 s isothermal y 2 een 2. )( W are the c subscript − the w − the propagation momen hampagne of v obtains GO of the e v 1 d Sh the 1 of the elo in the  for the will  gas the ∂ ∂ − ∂ results. the ∂ sho dR dx u dx dv VERNING the ρ t u these v t sho § cit ρ x ev elo self-gra (1977) the reduced + u ( self-gra tum + s 2 densit c cen flo discuss r cloud y = = ) ( k olution en c , r t and cit r u ‘u’ equation = k t 1 w ws , and 2 x reduced ) R 2 and tral x tire t ∂ ∂ x o expressions flo is y v ) equation, ∂ 1 = u r =  of (‘d’) , is y coupled = w vit v − § ws; at isothermal, vit = r ( densit r K ∂ system e at and the densit massiv x go a r 3 v av 2 n n. y r EQUA of s R R t in ρu y − − R , sho v resp ( finally = and indicates d u is tro erned of of x a ( self-similar densit
the ρ x u x 2 ) = 0 y )( c the y . = ) first the state duce ∂ is ectiv ∂ e k , for induces pressure n ( TIONS upstream ρ r stellar in 0 v star, and the , , − , u b y p cloud in th t order y ely; − osition equations 2) the R P > the us gas the an § x the − = 0. and s an equations winds similarit 5 in ) the core that n 2 differen- out con v v a SLGCL , w  elo (do alue expan- 2 § im , of v e ρ LIZANO jump w tin elo 4 cit (12) (11) (14) (13) (10) (15) bal- wn- and w will will ard the (8) (8) (9) in- w u- as of c- y y e , ET The the space tegrated found of r fulfilled. the x sho crossing F and densit jump w its ical line inner the of in densit R do sp x v the ences due and upp is dotted elo or 3. ard d AL. → terior → = R onds at es Fig. time a c Equation A F The Figure = ( er do LHS cen cit the OUTFLO to v p v k sho x densit R x latter or 0 ∞ t a erage x olume. osition from s condition y y in solution, ) 3 are wnstream in y where panel , the s the , the fairly , tral line . to 1 → = x ws 20 equation outer Fig. to giv ρ upp v = are the time similarit v of Once n sho → r R a ∝ for cloud y umerically 2 1. densit → r s b just en large the in origin, 2 sho zone b region equation s er . oundary = R in ws corresp 1 sho ∞ 56 terior t go exp (14) the and Except = n W solution, is − b n x Then, terior sho ws x panel for function y the n o x do = x (equation the w the and s smaller general . d ( reduced x y b of SOLUTIONS spreading at s (13) y jump wnstream ws for and at the . v 2. of x Z the job n = is This v reduced co elo the The and x onds reduced alue b GRADIENTS v the ev x b → uniform = The (14) uniform of the for condition that the x ordinates. oundary olume. lo out can cit of v s analogous enly x conditions H 2 cus expansion, Figure R than 0, is ( R u b and p . y of a x upstream v ironing w 99. densit reduced to asymptotic I s p osition v 0 15). = b the I → the ard  − = sligh of osition v anishes. ≡ the 3 e of ( v o region, the from ∞ v densit v elo R to x → but 1 in the 3( The dr and the er the high − 0 conditions b exp original + ) y F from tegrated 1 on t x/x and s the cit critical ( F nx/ /dt OR x = the out ev increase n of steadily expansion sho reduced n v rom the 0 critical sho dotted is y of ected (equation R y ) elo ( is reduced − aluated s gaseous R where 2 p n The the R 2 ) = 3 v ws R only enclosed DIFFERENT ost-sho x the 2 − v pressure implies x d 2) expansions c − cit b sho , u , . is equation 2 and k ax gaseous 1 = = whic sho where line. − = 1) the y as The  b lo kno sho in c s line decreasing are a line eha of 1. the can . v k n . 0 w 1 R c elo from . function pressure v er ph c time. h 02. reduced k, c fron dx wn, and R F 15) that k elo dashed k vior In v spher- ∝ in differ- or sound where cit b corre- ysical panel R v 0 x mass fron from ) e → cit (10) alue (16) (17) The s t this d y the the x the the are , for in- in- . as at n of y is is v 0 t , . Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México is dashed the The The Fig. Fig. is n n dashed the = only = v 1 deviation deviation sho 2 sho 1. 2. 2. = . 99. v line curv c T T c 1 1 The k k op op = . 02. The fron fron corresp 0 e p p . dotted anel: anel: from from 16. corresp t t Bottom dotted is is Bottom at onds at uniform uniform reduced reduced line x onds x line s s p = to anel: = is p 19 anel: is to R 2 densit densit the . v v . 56. the = 25. elo elo R reduced 300( critical cit cit reduced = The critical The y y . . y y 3( x/x SELF-SIMILAR v v x/x pre-sho pre-sho for for densit s line ) densit line s 2 ) . the the 99 2 v c c and v y and k k y exp exp = = R v v R elo elo . x x sho sho . onen onen − − The The cit cit ws ws 1. 1. y y t t CHAMP expand con the p p sho with similar at case sit sho pre-sho gaseous to b v the Fig. spatial p resp solid tio enclosed long-dashed p R sho alue er onen ost-sho er ost-sho d A y x /R the c of trast, c c Figure GNE and function k is ectiv R isothermal k k 3. = the line the u n from ts reduced x also in dynamics c . origin) x s mo k Results p lo b c c ; s mass One n ely; = osition the w sho FLO k k efore spherical p reduced sho the the . to dels er ost-sho the and the densit line The 2 3 ws c the lo and brok can . k pre-sho upp WS 99, in v is R summarizes w v the of a elo with sound pre-sho fron elo the sho terior er v there solid actual only = raises y en densities, see erage the er c the cities giv k cit panel ws sho v increase.  t p lines and olume. and differen c osition that y 3 en long-dashed mo is v k line the c to sp is − c u of k 3 exp p ( the k v at v dels lo has eed pre-sho sho ostsho = b elo n less arriv r d the reduced ratio x y w sho R s ,  ectation x the s 0 w er cit d t immediate v of = . s a spreading  as increases Fig. The /R of u 16, ws sho time p the es. ) y corresp dotted = x the x o c of x results a u the resp c k s w s of . the k c b at  19 p function er-la dashed the The k line 2 v v ecause ost-sho reduced sho n alue for the elo . 3 ectiv w H ev sho 25. , / p a p ondingly lines c (3 w cities I sho enly osition as v reduced ost-sho k the I gas for ws the do e R ely − densit region. x This n c line relativ ws at d wnstream of k s , n sho , densities that cloud → the (relativ o = and ( original ) and a v n the the v c er = of sho 368. . d w 3. k giv n y large , den- (18) self- um- e pre- The 300 169 and the the the the v up- ex- the ra- ws en In to to u e ) Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México instead wind. up the allo of the an where sno sure densit the will, 170 form where the the cause sion winds accelerates self-similar wind tion sp Gara radius sho n lar densit spatial (c flo the the ρ hampagne-dominated eed, ≥ w 4. mass ( shell, w-plo w arbitrary Massiv F t w winds sho analytic v sho wind sho stellar ) for or (wind-dominated ed 15) y 3, of elo r driving STELLAR can in p = y y the w In v et L r o r c assumed c c the co course, ery the that s of giv cit k s w conserv from the w = k k Z w the ( r imply al. our remain t er-la 0 ordinates mass-loss fron w = mo e v ) y inside the sp = r en  phase × , wind Z case and elo early mo s sho = wind stars (1994) increases, solution driv the x 3(3 0 eed 4 cen del constan the notation 1 2  r t the s π w c cit s M dels. at x L c and ev hampagne r ation, that ˙ 4 ev 125(3 k ter s n + solutions sho en 2 w WINDS , includes constan w y π tends at confined ev in c en 2 (Castor, ρ sho radius , are ( radius en hampagne accelerates = u r w π n ( x who b olv u n 2 tually w 2 r c their rate, the K ) e (equation is On s tually y , 3, s k t. x dr 2 R c a < t (7 momen is see exp k − s es a ) = ) the v the flo n equations to FLO = elo The dr 3. studied → hot sho the flo div the n − t.  with ax w). in of liv and INSIDE ected the C for )(9 that 1 inside the break flo assumptions cit McCra In instan w), n / o = to ∞ s erges. c x 5 es. bubble WS Comparing v other )(11 influence , k wind jump w 3 the y ertak tum, t − this  flo origin, go to the u (3+ a constan as and fron 18). whereas div for tends 3 w As 2 ws, to the medium the do n taneous + radius to ∞ − n y 3 (13) v case, is erges v ) hand, luminosit CHAMP ) es , t, and d conditions n sho v turn wn. / 2 alue If of n ev infinit & 5 w as the n c Th = where → , the  ≤ r to hampagne ) sho e one olution t r wn s and W  the energy ρ 0 r x us, of of as sp assume for 2 = b of 1 x , on s this stellar [ , for ea / r c c ecome . p of y where ab 5 the for hampagne the → s eed k the n in the equations x . osition v (14) ( A ed follo the n y Th p t er s the tegrates uniform o → , GNE )] SLGCL at o expres- ∞ v of sw n > (equa- stellar w stellar , mo M of of us, e, LIZANO sho 1975) , ˙ 3 pres- wind wing . erful ha stel- that case (19) (20) flo < ept- uni- C w and 2 the the the b del As c v in of e- w it is is k 3 e ET the transcenden v F F the where instead sumption 26 induced crease 10 t one 1 where wind-dominated u p the the lution x that c n nated stellar tion, densit c differ exact sho ypical hampagne-dominated hampagne ariable . or or w w o 62. AL. = 16 w km w = ' One In W the er-la cloud range sno a 2, previous g obtains equation equation e x 16 solution, y b s cm that Since H stellar the x linearly x of wind as − s y w-plo v distribution the densit w , s ha can w b I km 1 equation alues − less I i.e., ). = winds y exp of is b v of particular 1 region exp the y , actual e when tal s 2 uniform flo confined x giv x refine w − and parameters x . ected than 6 wind the s y w 56 discussed estimate. of 1 (20) onen (22), w π ws with equation x passage equation en ) = phase L = parameters inside K the w and remains w flo = lik passage a (10), 2 a found  densit b 5. = 10% r a ts this can at with . y w 6 time. obtained w with 56, ' e 3 ph densit 1 molecular π  case SUMMAR inside ( R n equation Orion . < the t equations 74, 18 is a 10 ysical c . ) ( flo one of b estimate . the hampagne 3 L x y (23), R = In for L the e π a b ( K km W giv L s inside w w The In the edges of L profile n ( y w ) y densit used a in x w x x particular, e can w the R 3 = stellar (equation p x as w of en = s terms SLGCL. ' the s 2 parameters s , using ) K are self-similar ossibly w ( for sho − go a K x 3 x (20) 2 condition opp 1 massiv 10 c .  Y t, core w then s 3 to b of the ) 20 , o y hampagne sho 1 giv b n R b y c therefore ) ' d / 36 one that k y slop oth  molecular 5 estimate ( of osed = the flo wind (see the 1 x for e, 54 (mo agreemen c . erg c relaxing / ) had hampagne write is k. the ws 2 3 e These 19), , e obtains established r for a mean . can and n s s steep ving ionized requiremen Fig. cores, to In giv − wind (mo of self-similar = an and to mo 1 n and confiden , a this en flo the k differen 2, the original eep and at ving 3). dels densit er = ha mo stellar- clouds. the t w, r ab domi- x using K w solu- v than u with w case 2, ev (24) (21) (23) (22) flo dels and e F o s the the as- for in- v at or in o- of ' ' = w y a a e t t t Winds, Bubbles, & Explosions: A Conference to Honour John Dyson. Pátzcuaro, Michoacán, México, 9-13 September 2002. Editors: S. J. Arthur & W. J. Henney © Copyright 2003: Instituto de Astronomía, Universidad Nacional Autónoma de México ionized heated that that c tion shell gas n sit tak et sup sion only the con et Photo ing ablation range up tion ha Williams, the Jorge gran Daniele Science main Susana F c NSF ac useful H p haracteristic hampagne rank ort > kno I v y al. al. I es tin One Apartado 04510 astro.it). (sh W e ersonic the b inside source cen t 2, p regions. of as measure tain exacerbate can y tra is from and e wledges v o 1994). the COFIN-2000. ev uous 10 Can 1994; [email protected] discussions. alues the Sh w the the tral thank a out it gas densit v problem Council. ap Galli: Lizano: 6 er-la b el u: of compact c cm M NASA, the t´ e wind p the oration & hampagne stellar DGAP o: fades expansion source photo star ossible at ´ exico, confined of to flo remnan Ric − National of w The Dyson P F of decreases y supp Instituto 6 high ws c Osserv constan equilibrium, rank ostal sup exp hampagne p shell the hling the of star-forming (e.g., found c a ev Instituto stellar erk A/UNAM wind D. and w of and, of D. ∼ ersonic < ort H onen S. the ap to a t situation. observ emission Wilkin 3-72, ionized eley y accelerates 1996) circumstellar EM inside G. I atorio F., sho L. oration of & I neutral in Lizano Tsing t tak in from b driv region. expanding t de in rapidly y .edu). ac c v and winds Y c the M ∼ hampagne n T < elo e k. SLGCL 58090 ork ed flo kno sp general, Astronom aiw ´ exico. en the are de ≤ 10 and in Astrofisico mass steep observ cit eeds. w. and J. 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