ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 28 September 2013.

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Presentation transcript:

ARE MAGNETIC FIELDS AND OUTFLOWS ALIGNED IN PROTOSTELLAR CORES? Chat Hull University of California, Berkeley Radio Astronomy Laboratory 28 September 2013 Academic Exchange Session: Physical Sciences & Mathematics 2013 Conference of Ford Fellows Washington, D.C.

Pereyra & Magalhães 2004 Large-scale: ordered fields 10 pc E,B Musca dark cloud

What is the role of magnetic fields in star formation? Fundamental? Nothing but a smiley face in the froth?

Credit: Bill Saxton, CfA

Girart+ 2006Rao Outflow B-field IRAS 16293NGC 1333-IRAS 4A Misalignment of B-fields and outflows

CARMA Combined Array for Research in Millimeter-wave Astronomy Consortium: Berkeley, Caltech, Illinois, Maryland, Chicago – 6 10-m, 9 6-m, m telescopes – Observations at 1 cm, 3 mm, and 1 mm (polarization!) – Located in Cedar Flat, CA (near Bishop)

Orthomode transducer SIS mixers WBA13 I.F. amplifiers (1-9 GHz ) 1 mm dual-polarization receivers 1 inch Credit: Dick Plambeck Waveguide circular polarizer

Girart+ 2006Rao Outflow B-field IRAS 16293NGC 1333-IRAS 4A Misalignment of B-fields and outflows

TADPOL survey

TADPOL collaboration UC Berkeley Chat Hull (PI), Dick Plambeck, Mel Wright, Carl Heiles, Geoff Bower University of Maryland Marc Pound, Alberto Bolatto, Katherine Jameson, Lee Mundy Caltech Thushara Pillai, John Carpenter, James Lamb, Nikolaus Volgenau University of Illinois, Urbana-Champagne Leslie Looney, Dick Crutcher, Nick Hakobian Other Dan Marrone (Arizona), Meredith Hughes (Wesleyan), John Vaillancourt & Göran Sandell (USRA-SOFIA), John Tobin (NRAO), Ian Stephens (BU), Jason Fiege & Erica Franzmann (Manitoba), Martin Houde (UWO, Caltech), Brenda Matthews (NRC-CNRC), Woojin Kwon (SRON)

TADPOL survey 37 sources Largest survey of star-forming cores to date >500 observing hours CARMA C, D, & E arrays 1 – 4" resolution 10 higher resolution than CSO & JCMT Probes intermediate region between ~0.1 pc (single-dish) and ~100 AU (ALMA)

TADPOL results L1157 See also: Stephens+ 2013, ApJL, 769, L15 2″

Credit: Bill Saxton, CfA

TADPOL results NGC 1333-IRAS 4ANGC 1333-IRAS 4B 2″ 4B 4B2

TADPOL results L1527NGC 1333-IRAS 2A 2″3″

TADPOL results Ser-emb 8 3″

CDF Outflow vs. B-field: distribution Simulation: outflows & B-fields aligned within a 20º cone (tightly aligned) Simulation: outflows & B-fields are randomly oriented KS-test results: 20º cone ruled out ( p-value ~ ) Misaligned ( 0.33 ) and random ( 0.33 ) cannot be ruled out Simulation: outflows & B-fields aligned between 70–90º (preferentially misaligned) Hull+ 2013a, ApJ, 768, 159 (plot updated Aug ‘13) outflow – B-field (deg)

B-fields are either preferentially misaligned (perp.) or randomly aligned with respect to outflows at the ~1000 AU scale Thus, circumstellar disks are misaligned with fields in the cores from which they formed Questions: Why are B-fields and outflows randomly aligned? What will disk-scale B-field measurements show? TADPOL outflows vs. B-fields: ApJ, 768, 159ApJ, 768, 159 TADPOL survey (CARMA key project): tadpol.astro.illinois.edutadpol.astro.illinois.edu Summary

Fin