List of Contents, The Star Formation Newsletter Interview 3. Perspective 6, Editor Bo Reipurth, reipurth ifa hawaii edu Abstracts of Newly Accepted Papers 12. Technical Assistant Hsi Wei Yen Abstracts of Newly Accepted Major Reviews 52. hwyen asiaa sinica edu tw Dissertation Abstracts 53. New Jobs 55, Editorial Board, Meetings 58, Joao Alves. Alan Boss Summary of Upcoming Meetings 64, Jerome Bouvier New Books 66. Lee Hartmann, Thomas Henning, Jes Jorgensen, Charles J Lada. Thijs Kouwenhoven Cover Picture, Michael R Meyer, Ralph Pudritz The Carina Nebula is a rich star forming region. Luis Felipe Rodr guez at a distance of about 2 3 kpc with about 65 O. Ewine van Dishoeck stars distributed in several clusters and producing. Hans Zinnecker powerful UV radiation that sculpts the surrounding. molecular clouds The image shows the dominant, The Star Formation Newsletter is a vehicle for northwestern cloud Eta Carinae is outside the left. fast distribution of information of interest for as edge of the image The Trumpler 14 cluster con. tronomers working on star and planet formation taining 10 O stars is seen in the upper left part of. and molecular clouds You can submit material the image. for the following sections Abstracts of recently, accepted papers only for papers sent to refereed Image courtesy Bastien Foucher. journals Abstracts of recently accepted major re http www bastienfoucher com. views not standard conference contributions Dis, sertation Abstracts presenting abstracts of new. Ph D dissertations Meetings announcing meet, ings broadly of interest to the star and planet for. mation and early solar system community New, Jobs advertising jobs specifically aimed towards Submitting your abstracts. persons within the areas of the Newsletter and, Short Announcements where you can inform or re Latex macros for submitting abstracts. quest information from the community Addition and dissertation abstracts by e mail to. ally the Newsletter brings short overview articles reipurth ifa hawaii edu are appended to. on objects of special interest physical processes or each Call for Abstracts You can also. theoretical results the early solar system as well submit via the Newsletter web inter. as occasional interviews face at http www2 ifa hawaii edu star. formation index cfm, Newsletter Archive, www ifa hawaii edu users reipurth newsletter htm. sumed had to be wrong since nobody else had pursued. them Then in 1978 I met Bart Bok who enthusiastically. Bo Reipurth supported me and gave me the courage to pursue these. in conversation with Hans Zinnecker ideas I went to my eclipsing binary advisor who expected. me to come with my finished thesis and instead I told him. I quit This caused much consternation but I stuck to my. decision and then with Bart Bok and a Danish expert on. the interstellar medium Jens Knude as dual advisors I. instead completed a thesis on Bok globules and showed. that they were remnants of dense cloud cores escavated. from more tenuous molecular clouds by the presence of. closeby massive stars I showed that globules indeed do. form stars but that they are only contributing a tiny frac. tion of all newborn stars Today that s widely accepted. and pretty self evident but it made quite a splash then. Q Soon you switched your interest to Herbig Haro jets. A As a teenager I read an article in Sky and Telescope on. mysterious semi stellar objects found in dark clouds that. might be related to the birth of stars I was mesmerized. Q With the present issue 300 of the Star Formation. and dreamt about one day studying such Herbig Haro ob. Newsletter you have edited the Newsletter for 25 years. jects As soon as the Danish 1 5m telescope at La Silla was. How did it start, equipped with a CCD in 1982 I started to image HH ob. A When I was a student in Copenhagen in the 1970s it jects My first scoop occurred on 20 December 1982 when. was not so easy to follow the latest developments in as I was imaging the HH 34 object In those days the read. tronomy as it is today The major libraries exchanged out and display was painfully slow so while I was looking. preprints which were especially important because pub at the image of HH 34 itself slowly this major finely colli. lication times were much longer in those days Only the mated jet rolled up above it one knot at a time I almost. largest institutes were reasonably well covered otherwise fell from my chair I had never seen anything like that So. if one had been lucky enough to hear about a new inter I embarked on a detailed multi wavelength study of this. esting preprint one had to write the author and receive object and soon others. a copy by postal mail So by the early 1990s when email. Q You have made many surveys for new Herbig Haro ob. had become universal I one day had the epiphany that. jects Do you have any favorites, one could make a newsletter with abstracts distributed. by email and so I created what was the first electronic A When I was young I was frequently observing at La. newsletter in astronomy every month calling for and col Silla and whenever the weather was bad I would spend. lating abstracts of newly accepted papers on Galactic star the night poring over the large sky atlas films which were. formation and young stars With time the Newsletter has at that time being produced at the ESO and Siding Spring. evolved bringing additional information relevant for our Schmidt telescopes It was an excellent way to become. community Still the Newsletter is not as indispensable familiar with the known star forming regions but to my. as it was once and every month when I have to find time surprise I kept finding objects that were not described any. to assemble another issue I think about shutting it down where so of course I started studying them That way I. But I regularly get nice emails from people who like their found numerous new HH objects I have lost count But. monthly issue and thank me for the effort so I continue one object stands out namely the HH 111 jet which I. found later after I in 1986 moved to Chile to become a. Q Your earliest work was on Bok globules, staff astronomer at La Silla a position I held for 11 years. A I actually started doing a thesis on eclipsing binaries I was curious about a little studied region of Orion and. which was the main focus of Danish astronomers in the requested a deep photographic plate of that area I saw. 60s and 70s But my heart was really beating for star for on the plate a little streak in a dark cloud and the same. mation and I read all the papers on the subject which evening I got very excited when my CCD images revealed. was possible back then but certainly not today I was a beautiful and perfectly collimated bipolar jet emerging. fascinated by Bok globules which in the early days were from a dense cloud core I have spent several years study. seen as an intermediate stage in the contraction of the in ing this object with many techniques and at many wave. terstellar medium into stars I had some what seemed lengths and the object has generated much interest and. to me simple ideas about their formation which I as is in many ways a benchmark for jet studies By now well. over 50 papers have been devoted to it by many groups Q 30 years ago you wrote an early review on pre main. Later I noted two large HH shocks far from and symmet sequence binaries an interest you have maintained during. ric around the HH 111 source and I realized that HH 111 all those years How did that start. formed a giant bipolar HH complex almost 8 parsec in A Well as I mentioned earlier I started out working on. extent From this emerged a major study of giant parsec eclipsing binaries and it was therefore natural to ponder. scale HH flows that I wrote with John Bally and his stu the formation of binaries The first step was to identify. dent Dave Devine Giant flows have dynamical ages com and characterize a large population of young low mass bi. parable to the duration of the main accretion phase of the naries So I embarked on a massive imaging survey of more. sources and thus provide a fossil record of their mass loss than 200 T Tauri stars doing 1 m CCD imaging at the. and accretion history Such giant flows have burst out of NTT in sub arcsec seeing and that was the genesis of the. their cloud cores dissociating molecules and injecting mo large paper that you and I published in 1993 Within a. mentum and kinetic energy into the interclump medium of month the speckle interferometric studies of Leinert et al. the host clouds They may contribute to the chemical re and Ghez et al appeared and all three studies showed a. juvenation of clouds the generation of turbulent motions clear excess of binaries in star forming regions compared to. and perhaps even the self regulation of star formation the field pointing to powerful dynamical processes shap. Q You also studied the driving sources of these HH flows ing the early separation distribution function. A Infrared astronomy was in its infancy in the 1970s and Q In 2001 you and Cathie Clarke suggested that brown. we had little idea what was inside most molecular clouds dwarfs may be ejected stellar embryos from disintegrating. so already as a student in the late 1970s I started groping triple systems What was the origin of that idea. around in the clouds surrounding HH objects trying to A This was a corollary to a study I had done the year be. identify their energy sources This was with single pixel fore where I pointed out the very high fraction of higher. InSb detectors with which one made manual raster scans order multiples among the driving sources of HH flows I. across the selected regions a laborious process which is found that the structure of giant HH flows could be under. hard to imagine now that we have widefield near infrared stood in terms of the orbital evolution of a binary newly. imagers and various all sky infrared catalogs Such sur formed in a triple disintegration event Such breakups. veys together with later surveys that Rolf Chini and I of T Tauri stars had been previously studied numerically. did in the early 1990s at submm wavelengths identified especially by Michael Sterzik and it was clear that the. a number of the flow sources known today and revealed lowest mass objects were most likely to be ejected Cathie. that HH flows can take place at all evolutionary phases and I turned that around and pointed out that brown. from Class 0 to Class III dwarfs are of low mass precisely because they are ejected. Q What about jets from massive stars In other words when a stellar embryo is evicted from its. nascent cloud core it is deprived of the mass that it needs. Herbig Haro flows are rarely found in association with to eventually be able to burn hydrogen It has come as a. massive stars And in the few cases known they tend surprise to me that it has taken the community a while. to be poorly collimated not jets One spectacular ex to embrace this simple idea After all there is no voodoo. ception is the HH 80 81 flow In the early 1980s I was physics involved just straight dynamics The question to. interested in objective prism surveys in the grand tradi ask is not whether this mechanism operates because it is. tion of Guillermo Haro and George Herbig I used the inevitable but rather what fraction of brown dwarfs are. Curtis Schmidt at Cerro Tololo which required guiding at formed this way compared to other processes that also. the eyepiece for 4 hour exposures and ending the night will lead to very low mass objects. in the dark room developing the plates I remember one. morning holding a wet plate up to the light and seeing Q You introduced the concept of Orphaned Protostars. the spectra of a pair of bright HH objects in Sagittar A In recent years I have mainly focused on studying small. ius These were the now famous HH 80 81 objects the multiple systems of 3 or 4 young stars both observation. most luminous known HH objects The driving source is ally as well as numerically It was Richard Larson who. the 104 L embedded IRAS source 18162 2048 Subse from an angular momentum point of view in 1972 first. quently Josep Mart Luis Felipe Rodr guez and I used stressed that it is likely that most stars are born in such. the VLA to detect a finely collimated radio continuum jet systems only to subsequently break apart If this is so. emanating from this newborn massive star The rarity of and the evidence increasingly points in that direction then. such jets from massive stars suggests that the collimation dynamics plays a much more important role than is rec. mechanism presumably by magnetic fields anchored in a ognized now Three body interactions can both trigger. circumstellar disk does not survive the intense radiation accretion as well as truncate some of the circumstellar gas. for very long reservoirs so dynamics is a stochastic parameter that can. influence the accretion history of young stars and affect A I enjoy writing The new book about George Herbig. the shape of the initial mass function I am convinced was a labor of love since I knew George very well person. that until we fully appreciate the importance of early dy ally and scientifically and I was always amazed at how he. namical evolution of such small N systems we are missing had almost singlehandedly opened the field of early stel. an essential element in early stellar evolution lar evolution with instrumentation that we would sneer. The Star Formation Newsletter is a vehicle for fast distribution of information of interest for as tronomers working on star and planet formation and molecular clouds You can submit material for the following sections Abstracts of recently accepted papers only for papers sent to refereed journals Abstracts of recently accepted major re
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Star Formation Studying the STAR FORMATION HISTORY temporal evolution of the star formation is key in understanding galaxy evolution in its broader context Two different models of galaxy formation and evolution MONOLITHIC simultaneous formation of structures from primordial fluctuations of densities subsequent fragmentation e g Eggen et
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the United States military formation training protocols and as such is not copyrighted Any individual or orga nization is welcomed to copy adapt and modify the con tent of this manual to suit their needs FAST assumes no responsibility or liability for the use of this material in part or in whole INTRODUCTION PREFACE F ormation flight dates back to World War I when the military began
Gully formation on Mars Two recent phases of formation suggested by links between morphology slope orientation and insolation history Gareth A Morgana James W Heada Fran ois Forgetb Jean Baptiste Madeleineb Aymeric Spigab a Department of Geological Sciences Brown University Providence RI 02912 USA bLaboratoire de Meteorologie Dynamique Universit Jussieu Paris VI Case postale
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correlation with other quantities such as stellar or gas masses Constraining the rate at which galaxies form stars across the Universe is of utmost importance if we want to understand galaxy formation and evolution 1 Introduction One of the most complex processes in galaxies is star formation and understanding it and its evolution with time remains a challenge for modern astronomy The
11 4 Formation of Stars Like the Sun Star formation happens when part of a dust cloud begins to contract under its own gravitational force as it collapses the center becomes hotter and hotter until nuclear fusion begins in the core 11 4 Formation of Stars Like the Sun When looking at just a few atoms the gravitational force is nowhere near strong enough to overcome the random thermal
Star formation in galaxy clusters Chiara Ferrari Post doc at the Institute for Astro and Particle Physics of Innsbruck University Lyon 7 9 novembre 2007 Formation et volution des galaxies dans la perspective de MUSE 2 24 Galaxy evolution vs environment amp z Increasing fraction of red galaxies with density 10 30 in the lower density environments Balogh et al 2004 70 in the
Star and Planet Formation Galaxy Evolution Investigating the gas in the Galactic Bar the missing link between the Galactic Disc and the Central Molecular Zone Natalie Butter eld Ashley Barnes Mattia Sormani H Perry Hatch eld Contact Person Natalie Butter eld Green Bank Observatory 155 Observatory Rd P O Box 2 Green Bank WV 24944 email nbutterf nrao edu Executive Summary The goal