Formation of protomultiple systems in a magnetized fragmenting
- Slides: 24
Formation of proto-multiple systems in a magnetized, fragmenting filament Credit: ESO/S. Guisard – http: //www. eso. org/public/images/potw 1217 a Chat Hull Center for Astrophysics Jansky Fellow —Harvard-Smithsonian National Radio Astronomy Observatory 20 November 2015 Postdoc Symposium Harvard-Smithsonian Center for Astrophysics Cambridge, Mass.
Intro: Magnetized star formation Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 2
B-fields in largescale filaments Musca dark cloud 10 pc B E, Pereyra & Magalhães 2004 Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 3
Polarization (via dust absorption) ALIGNED DUST GRAINS ORDERED MAGNETIC FIELD BACKGROUND STAR (unpolarized) Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 4
B-fields in largescale filaments Musca dark cloud 10 pc B E, Pereyra & Magalhães 2004 Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 5
B-fields in largescale filaments Musca dark cloud 10 pc B E, Pereyra & Magalhães 2004 XX k c n a Pl Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 XIII, 6
Polarization (dust emission) ALIGNED DUST GRAINS ORDERED MAGNETIC FIELD Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 7
Credit: Bill Saxton, NRAO/AUI KALYPSO project, Harvard/Cf. A
What is the role of magnetic fields in star formation? Incidental? Fundamental? Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 9
Magnetized filaments Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 10
Magnetized filaments Low-mass star-forming cores Ser-emb 8, 8(N) Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 11
Ser-emb 8, 8(N) 0. 01 pc • This filament is small! (d ~ 0. 01 pc) • How did this filament form? • What does the B-field look like in (and between) the cores? Hull+2014, Ap. JS, 213, 13 Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 12
ALMA Credit: ESO/S. Guisard – Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 13
Filament: Ser-emb 8, 8(N) CARMA Dust continuum 1. 3 mm (230 GHz) d = 429 pc beam ~ 3ʺ (1300 AU) 5000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 14
Filament: Ser-emb 8, 8(N) ALMA Dust continuum 1. 3 mm (230 GHz) d = 429 pc beam ~ 1ʺ (850 AU) 5000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 15
Filament: Ser-emb 8, 8(N) ALMA Dust continuum 1. 3 mm (230 GHz) d = 429 pc beam ~ 0. 5ʺ (215 AU) 5000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 16
Filament: Ser-emb 8, 8(N) ALMA Dust continuum 1. 3 mm (230 GHz) d = 429 pc beam ~ 0. 36ʺ (150 AU) 5000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 17
Proto-multiples? 400 AU Blob masses ~ 5 -10 Mjup Ser-emb 8 400 AU Ser-emb 8(N) Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 18
ALMA continuum + CARMA B-fields Ser-emb 8, 8(N) 2000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 19
ALMA continuum + CARMA B-fields Ser-emb 8, 8(N) 2000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 20
ALMA continuum + CARMA B-fields Ser-emb 8, 8(N) The filamentary blobs are parallel to the 1000 -AU-scale B -fields! 2000 AU Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 21
Filaments, B-fields, and blobs (oh my!) • Implications for the formation of multiples – Do we expect such uneven fragmentation? • What will the B-fields look like in the filamentary blobs? – Consistent with 1000 AU B-fields? • What will the B-fields look like at hi-res in the cores? – Toroidally wrapped? Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 22
Summary (1) Fragmentation at ~400 AU scales near low-mass protostars (2) B-fields (CARMA) & blobs (ALMA) have consistent orientations (3) What will the ALMA polarization results show? Stay tuned… More info chathull. com Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 23
Fin Chat Hull – Cf. A Postdoc Symposium – 20 Nov 2015 24
