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Modified and pure dynamo field in nearby galaxies Krzysztof Chyży (Jagiellonian University, Kraków)

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Presentation on theme: "Modified and pure dynamo field in nearby galaxies Krzysztof Chyży (Jagiellonian University, Kraków)"— Presentation transcript:

1 Modified and pure dynamo field in nearby galaxies Krzysztof Chyży (Jagiellonian University, Kraków)

2 Outline A disturbed galaxy NGC 4254 in the Virgo cluster  The disturbed magnetic field and the idea of „magnetic maps”  Correlations between the magnetic field components (B reg, B ran, B tot ) and the local SFR  Are the magnetic fields modified by ram-pressure or tidal forces? An isolated, early-type galaxy of ringed morphology - NGC 4736  The observed structure of magnetic field in the inner ring (the Lindblad resonance)  „Pure” dynamo – without support from spiral density waves In collaboration with R. Beck, R. Buta, M. Ehle

3 Outer magnetic arm Chyży, Ehle & Beck 2007, A&A, 474, 415 VLA+EFF 4.86 GHz (6.3cm) NGC 4254 Virgo cluster spiral, weakly disturbed

4 NGC 4254 PI 4.86 GHz The ram-pressure of the cluster gas - compression? (anisotropic random field?) Vir A 1.2 Mpc

5 HI (WSRT) - VIRGOHI 21 (Minchin et al. 2007) The tidal interaction - stretching/shearing (anisotropic random field)? A range of HI blobs. The largest one: M=10 8 HI data cube (xyv) Ram-pressure or tidal interaction? Vir A

6 Magnetic maps (B corrected for projection and Faraday rotation) Chyży 2008, A&A in press, astro-ph 0712.4175 Projection i=42 o P.A.=68 o TP PI polar. angle Farad. rot. (from 3 and 6 cm data)

7 The modelling of compression (ram-pressure) and stretching (tidal effects) in the polarized ridge B 2 tot = B 2 reg +B 2 ran = B 2 coh +B 2 ani +B 2 ran Compression – enhances B ran too much! Stretching well corresponds => tidal interaction stretching/shearingcompression - geometry of the ridge and acting forces - scaling of the field components following Sokoloff et al. (1998), Beck et al. (2005) degree of polarization intensity ratio B-components – a sensitive tool to reveal physical processes! Chyży 2008, A&A in press, astro-ph 0712.4175

8 Magnetic field components - SFR

9 Why the field regularity anicorrelates with SFR?  Tangling/disruption of the regular field in the regions of enhanced star formation (by turbulence)  Production of turbulent (random) field proportional to SFR  Production of regular field antiproportional to SFR correlation length of turbulence antiproportional to SFR (Rohde 1999) turbulent diffusivity enhanced by shearing (Moss 2001, 2007) suppresion of the mean-field dynamo in the spiral arms (Shukurov 2005) MHD simulations needed!

10 Ringed galaxy NGC 4736 Early type Sab The large oval causing outer and inner Lindblad resonances => mass accumulation The outer ring – very weak The inner ring – well-defined zone of star formation Flocculent spiral pattern Circular gas motions 200 km/s Magnetic field? UV opt Waller et al. 2001

11 NGC 4736 radio contours at 8.5 GHz (VLA+EFF) infrared 24  m – colors (SPITZER) 8”x8” (200pc x 200pc)

12 NGC 4736 Chyży and Buta 2008, ApJLetters, in press, astro-ph 0803.0555 Polarized intensity 8.5 GHz + B (of PP) Hα image rms=6μJy

13 Magnetic field vectors do ignore the ringed morphology altogether! large p=35 o Undistorted dynamo? - B reg in the galaxy’s plane, free of projection effects - contours of PI - Hα image in colors

14 NGC 4736 Sombrero B tot 30  G 6  G B reg 13  G 3  G Sombrero (Sa) Krause et al. 2006 The dynamo process must be very efficient! Magnetic field strength B tot B ran B reg NGC 4736 – B stronger than in typical spirals (Beck et al. 1996)

15 r  =440 pc, v=200 km/s – rotation curve of CO and HI (Wong & Blitz 2000)  T = 1kpc km/s, h=500 pc – typical values for spirals (Elstner 2005, Shukurov 2005) => pitch angle p=2 o (instead of 35 o ) thinner disk or larger turbulent diffusion (>10 kpc km/s) Parker instability? MRI? Magnetic pitch angle in NGC 4736 According to Elstner (2005)

16 Summary NGC 4254 Its magnetic fields are disturbed and match density waves The total and random fields correlate but the field regularity anticorrelates with SFR, while the regular field very weakly depends on SFR The magnetic field components discriminate between the tidal and ram-pressure effects NGC 4736 Its radio emission closely associated with the inner ring B reg ignores the galaxy’s ring and shows a spiral structure Magnetic vectors cross the ring at large pitch angle values – large turbulent diffusion? Strong fields (efficient dynamo) in early-type galaxy A challenge for the dynamo theories and simulations! (?)


18 Regular field pattern in NGC 4254 B corrected for Faraday rotation Coherent structure – matching the density waves




22 Other wavebands X (XMM) – contours Hα - image HI (VLA archive) - image 1.4 GHz - contours, + B (PI)


24 + Effelsberg AIPS + NOD + MIRIAD 8.5, 4.8 GHz (3, 6 cm) Radio polarimetric observations: VLA

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