Structures, accretion and ejection in protoplanetary discs

00 .Thecolorscaleisarbitrary. a. 2 functionassumingthattheuncertaintyon. theFWHM .... Transport angular momentum in the bulk of the disc. Suggested by ...
42MB taille 2 téléchargements 312 vues
is J A -th m m e size ) within e ized 9 n 4 s T . o ( 2 nd ak ( n a e a l h U r t , p h r e a t a 0 A l v (ME mstel 80 t is less a 3s le 1). The of ~39 osite u c o t d r S exten ed flux a rt (fig. noise rati n the opp The he ci s stymie o ct pa nd 0. si tooces l drift a te dete northern h signal- per limit or of 13 rth of ia ct ia ig no up e e rad intermed = th a very h ith the least a fa n in the ke the w s U a io f es o U) (1 A n), ha contrast ring is at ust emiss ntrast m earlier u e o d (A an unit h to the S igh th e of the sence of g high c treme th l slope B n rt ex Lesur tra (IPAG, sid lete ab iGeoffroy Grenoble) eh a t c r e l i E e r m u u o p s o q m omp and re feature m ). The s 4 mm c 4)] r] ac ect to the c a t s .4 13 48 d (1 or the th resp 0 e , f [ n p S 0 s a s R 1 h I i t-s lem es ( luxes F n quencie ng that n i e r t c s e sltLaer w jor prob llisions with (IPAG), Jonathan Ferreira (IPAG), cre fre e esti mm William er f Bethune tm t tea r h g y rs, 748:Ly co e t e s g a s u m w a ), s lo wo ate he & Matt Kunz (Princeton) cit22 (7pepl)o, 2c0i1ti2eApr dustSébastien illi sFromang t o n l a m i (CEA Saclay) n e e m v il t e v 1 o º th x h, s d t r e g u f f l e i l i f n r o c ) F v h i ( d , art ft a d with nt 25 ins (15 . Howe same p . e r 0 f i e i f T e dr in dif , even 67 ed gra mission rom the prob y . l 2 d i y p f a e z nd nl ey Seco ey will r efore th s is o meter-si tinuum 6-5 line rian disk inner Muto et al. b n li le th hi 12 it on, o the star size. T nt mil -mm co the CO es a Kep with 1a2n O 6-5 al C at te 44 nt isk by lost i anetesim st persis ble 0. s traced set indic a gas d g. 1B). radius, pl ssi mo (Fi 0 AU of ga ata o d r o e t c p a i h t AU t t A s e s 2 A w 0 f i l r r M 3 . a o u a C r e s t s L t t a n c A to ne heorie es e a e g r o r c n n p a m i s e r i o h w t r le c round th cted do hot CO ed still s op on t o-called the dus i i f t a y a is dete the is inde cant dr t i form ing in s where mp h v t u i a A& b c . w fi e e i n a t p r U r n o e n p u i m A A e t g h a i s t s i t s r s s t 5 is t u is ax 57 s re a d a T n m h p m t o e h 5 p 8, a t c s e i a 2 m r r e s h ~ u t t i w u L6 c a u s f , h c u n s n o i e c i s a l e i t d e c f o h n n (20 pr d i h o o . i w h ) c s e t s e c i 0 s l n v i i i h 15 1 u d p t h / T – d a n y l r m w t a 6 . i ) e a e e ) ( s , r t x h 4 m e n t x e n e 1 n e e e ( o i t e m i l h i d r t t i d d l o i c v il A res pla ut ace ire ins CO gas surf inuFisg. 2ALM oubt abo lonic uthal d arge M ort a high sub pect ne t e g r a L l d e im p ewo dica . Bneo d e h z An mil ivel emp e t t n z a r a i a a f s t e h e l o m h me t pe drew lime y, sli eratu t imu s lietharva eted b st-ufitsmt. y taca MA), w illimeter star s s a a c A i e n d diud ydw o a Su ratur s e ter c ghtl res n e Th vation i h n r t i the ray (AL n of m e d n s s t f a o 0.2 hittehuel i ed crome r t a 2gas ob ch a e m t al. onti y hi of ⇠ n e u o r k o s i b s t s c n i b 0 i A 5 r a 31 . Th serv hig easu 201 nuu gher n eter oncentr of the d 5 GHz) can o sitiontheoFf fuenrvation 0. Taherdeiamdoidsatshe mall mi ing. To s5 a m r h 1 i o t e s b i r su ili di d ), vamt ha c r e i s c r s s n th o d o s 8 n a W e b n t i e p th d c e i c t 6 s i e o a m i h d oloths. lin t th ongra thfoar the same FOV showAlthethe gge ty of sk as woibthsebrut s owdeitl hn tA anhe ete HM t esu d metr n one si 44-mm ( ue that t pping a r s Theho m T e a F h s S z t P d . i r i s m mn coalug sd theTh1.3ha digni ing t co feoters-sar of sbuu e g a . (e) and (f) or. Ttehrena spir sts thd tgheas pec sC n O o r v r ls e 0 t w r o n a o a r c i m h e P o s s e e . t t ) ) e r r s h , d t e ( t 4 e a u in is n tm tesdimliloac r ptarttiebrn rLehTe apu. irPnegaandel t us l amn at aspsirob rat (⇠5e sfitcaar th esp the oceftu W SEillirm α error