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246 — 7 June 2013 Editor: Bo Reipurth (Reipurth@Ifa.Hawaii.Edu) List of Contents THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar/planetary evolution and molecular clouds No. 246 — 7 June 2013 Editor: Bo Reipurth ([email protected]) List of Contents The Star Formation Newsletter Interview ...................................... 3 My Favorite Object ............................ 6 Editor: Bo Reipurth [email protected] Perspective ................................... 10 Technical Editor: Eli Bressert Abstracts of Newly Accepted Papers .......... 14 [email protected] Abstracts of Newly Accepted Major Reviews . 51 Technical Assistant: Hsi-Wei Yen Dissertation Abstracts ........................ 53 [email protected] Meetings ..................................... 56 Editorial Board Short Announcements ........................ 58 Joao Alves Alan Boss Jerome Bouvier Lee Hartmann Cover Picture Thomas Henning Paul Ho NGC 7822 is an HII region, also known as Sharp- Jes Jorgensen less 171, and located in Cepheus at the relatively Charles J. Lada close distance of 800 - 1000 pc. The central cluster Thijs Kouwenhoven is known as Berkeley 59. Parts of the complex are Michael R. Meyer as young as 1-2 million years. The dominant ultra- Ralph Pudritz ◦ violet source is the O5V star BD+66 1673, which Luis Felipe Rodr´ıguez is an eclipsing binary. Ewine van Dishoeck Hans Zinnecker Image courtesy Martin Pugh. 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 Submitting your abstracts accepted papers (only for papers sent to refereed journals), Abstracts of recently accepted major re- Latex macros for submitting abstracts views (not standard conference contributions), Dis- and dissertation abstracts (by e-mail to sertation Abstracts (presenting abstracts of new [email protected]) are appended to Ph.D dissertations), Meetings (announcing meet- each Call for Abstracts. You can also ings broadly of interest to the star and planet for- submit via the Newsletter web inter- mation and early solar system community), New face at http://www2.ifa.hawaii.edu/star- Jobs (advertising jobs specifically aimed towards formation/index.cfm persons within the areas of the Newsletter), and Short Announcements (where you can inform or re- quest information from the community). Addition- ally, the Newsletter brings short overview articles on objects of special interest, physical processes or theoretical results, the early solar system, as well as occasional interviews. Newsletter Archive www.ifa.hawaii.edu/users/reipurth/newsletter.htm 2 Q: Didn’t you also develop and coin the term ”competitive accretion” as a theoretical model for the IMF? Hans Zinnecker A: I guess this is correct. In my 1981 thesis I did two mod- in conversation with Bo Reipurth els of the IMF, the log-normal model (originally based on the concept of hierarchical fragmentation) and a power- law model (based on nonlinear Bondi-type gravitational accretion onto seed stars which were accreting from a lim- ited protocluster gas reservoir, hence the competition for gas accretion). This latter model was published in 1982 in the Proc. of the Henry Draper Symposium on the Orion Nebula and was popularized by Richard Larson who kindly quoted my work. Had it not been for Richard, no-one might have taken notice of that model. Now it is one of my most cited papers. Thank you, Richard. Q: You were a theorist at heart, how come you turned into a quasi-observational astronomer? A: Yes, I started as a theorist, influenced by Prof. Kip- penhahn, and also by talking to Profs Bodenheimer and Q: Hans, we have known each other for a long time, 30 Tscharnuter. Mind you, before my PhD in astrophysics I years, since the Les Houches school ”Birth and Infancy got a diploma in physics in conformal quantum field the- of Stars”. How influential was that two week school in ory - if anybody in astronomy knows what that is. After August 1983 in the French Alps? looking around, I ended up for my thesis work in a group of A: Very influential for many of us, myself included. It far-infrared astronomers (balloon observations) at MPE in was there that long-term friendships among many young Garching, headed by Dr. Drapatz (my PhD thesis advisor astronomers were initiated. I vividly remember meet- who taught me back-of-the envelope calculations). That ing John Bally, you Bo, Bruce Elmegreen, Gareth Wynn- environment helped me to get a sense for observations and Williams, Harold Yorke, to name but a few. Many of them that the best astronomy is often done in interaction be- for the first time. This was the time when molecular out- tween theory and observations. flows were first discovered, as well as the proper motions Q: You did your postdoc years at the Royal Observatory of Herbig-Haro objects, and I particularly recall discus- Edinburgh. How did that happen? sions with George Herbig. It was also the time when the first results from the IRAS satellite began to appear, and A: Interesting story. Coincidences. After my PhD I took a during the time of the school Bart Bok died in Tucson, trip to Hawaii and managed to force my way up to UKIRT AZ, making us feel that a baton was passed to the young on Mauna Kea (ask Eric Becklin about that particular generation. facet). At Hale Pohaku (the dormitory halfway up the mountain, quite rudimentary in 1981) I happened to meet Q: You presented your thesis work, a theoretical model of Gerry Gilmore (then at ROE) and gave him a copy of my the log-normal IMF in Les Houches, didn’t you? thesis (in German). Next thing I hear, after being back A: Yes indeed. I gave a presentation on star formation as a in Garching, was that Malcolm Longair (then director at random multiplicative process. The idea was that several ROE) who was visiting ESO Garching for a colloquium, factors determine the critical protostellar mass, such as had asked my advisor to see him before his departure. temperature, density, magnetic flux, angular momentum, Indeed I met with Malcolm and he offered me to come to geometry, etc in a multiplicative fashion. By and large ROE as a postdoc, on the basis of a mixed Royal Society this model is still valid (Fred Adams introduced outflows and German Science Foundation fellowship. I stayed for in 1996) and Basu and Jones (2004) as well as Phil Myers almost 4 years. This was a crucial move to turn me from (2011) realized how to turn the high-mass lognormal tail theory to observations. into a (Salpeter) power-law slope by adding the idea that Q: Can you elaborate a little more? the accretion time is uniformly distributed. Perhaps my own contribution here was to realize that for a log-normal A:. I try. At ROE, I met Tom Geballe with whom I did IMF that turns down below a certain characteristic mass, my first observing proposal (Brackett alpha in the Orion the predicted number of brown dwarfs (or black dwarfs as Nebula), Mark McCaughrean and John Rayner, both PhD these objects were then called) is small, i.e. the numbers students of Dr. Ian McLean, as well as Colin Aspin, Mike do not diverge towards small masses, as an extrapolated Burton, Ron Garden, and others. This reads like a who is Salpeter low-mass IMF would imply. who in infrared arrays at the time (Ian McLean heading 3 the IR-CAM development). I also there met Eric Becklin a co-author and Ghez et al.). This was a great month for (on sabbatical) and Steve Beckwith (colloquium speaker), me and in fact for young binary star research. who alerted me to high angular resolution observations Q:: In 1994, you discovered the beautiful HH212 molecular (lunar occultations and infrared speckle interferometry, re- hydrogen jet. How did this discovery come about? spectively). Which I later applied to studies of pre-Main Sequence binaries (originally with Chelli and Perrier 1986 A: Another interesting story which incidentally is con- at ESO Chile and later with Leinert and Haas 1990 at nected to my deep interest in binary protostars. In 1987, Calar Alto). This exposure to infrared technology led to in the early days of IR-arrays, I was interested in near- 20 or so visits to Mauna Kea during my stay at ROE, infrared imaging of cold, low-luminosity IRAS sources, which helped anchor my connection to observational as- in the hope to discover double stars in the same cloud tronomy. core, indicative of their joint formation (which was not yet proven at the time). IRAS 05413-0104 in Orion B Q: Apropos binaries. How did you get interested in pre- indeed showed two K-band near-infrared embedded point MS binaries? sources, about 7 arcsec (300 AU) apart. Nothing hap- A: When I arrived in Edinburgh in August 1983, I had just pened until 7 years later, when persistence paid off. My come back from an IAU Colloquium on binarity and a total colleagues Mark McCaughrean and John Rayner (with solar eclipse in Indonesia. I had to write a report for the me as a co-investigator) were observing the Orion Neb- German funding agency. This developed into a review on ula Cluster with a new and better infrared array at the binary statistics and star formation. Binary star formation IRTF on Mauna Kea. Mark ran into a software problem (mass ratios) clearly was the next logical step, after deal- related to the programming of the array mosaic pattern ing with the possible origin of stellar masses. Everything and said: ”I need to fix this. You can have the telescope in those days was kind of pristine territory in the young for the next 10 min”.
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