SMALL SCALE SOLAR MAGNETIC FIELDS. M. J. Martínez González Instituto de Astrofísica de Canarias

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1 SMALL SCALE SOLAR MAGNETIC FIELDS M. J. Martínez González Instituto de Astrofísica de Canarias

2 The Sun, the only star under the microscope Network φ 10 2 G B 10 3 G D 10 4 km Very quiet Sun φ 10 G B 10 2 G D 10 3 km Active regions φ 10 3 G B 10 3 G D 10 5 km

3 Small scale fields are most of the Sun, most of the time At the minimum of activity the Sun still mantains, e.g., the million degree corona

4 Which is the origin of these fields? Which is their role on the global magnetism?

5 When interpreting polarisation signals, we mostly agree

6 When interpreting polarisation signals, we mostly agree The very quiet Sun is alike everywhere Orozco Suárez & Katsukawa 2012, ApJ, 746, 182 Hinode data at 630 nm Martínez González et al. 2008, A&A, 479, 229 data at 1.5 μm See also Lites et al. 2008, ApJ, 672, 1237

7 When interpreting polarisation signals, we mostly agree The smallest the polarimetric signal, the smallest the spatial coherence < Bz > L 1 Martínez González et al. 2010, ApJ, 711, 57L Sánchez Almeida & Martínez González 2011, ASP, 437 See also Stenflo 2010, A&A, 517, 37

8 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops Extended tails are indicators of INTERMITTENCY: Events having a certain correlation length (organised structures) that have a low probability to occur but still very large as compared to the probability expected from an uncorrelated (gaussian) case.

9 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops The apex: linear pol. < > transverse field The footpoints: circular pol. < > longitudinal field Martínez González, M. J. 2006, PhD thesis Martínez González et al. 2007, A&A, 469, L39 Staple like loops

10 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops 2000 km Centeno et al. 2007, ApJ, 666, 137 Martínez González & Bellot Rubio 2009, ApJ, 700, 1391 Gömöry et al. 2010, A&A, 511, 14

11 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers Photosphere Minimum T Low chromosphere t=180 s

12 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers Photosphere Minimum T Low chromosphere t=180 s t=780 s

13 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers Gömöry et al. 2013, A&A, 556, 7

14 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers they do not appear uniformly in the solar surface Martínez González et al. 2012, ApJ, 755, 175

15 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers they do not appear uniformly in the solar surface Stangalini 2014, A&A, 561, 6 Martínez González et al. 2012, ApJ, 755, 175 Possibly related to supergranulation

16 When interpreting polarisation signals, we mostly agree Newly emerged flux in the photosphere, appears in form of intermittent, organised Ω loops they reach higher layers they do not appear uniformly in the solar surface they are the lowest fluxes of the solar flux power law distribution Martínez González et al. 2012, ApJ, 755, 175 Parnell et al. 2009, ApJ, 698, 75

17 In conclusion The newly emerged flux in the quiet Sun seems a similar phenomenon than the emergence in active regions: 1) The topology of the magnetic fields is similar 2) Some of them rise to higher layers and have similar imprints in the chromosphere (e.g. dark cold bubbles) 3) They are the lowest fluxes of the power law extending over five decades of flux (Parnell et al. 2009) 4) They do not appear totally uniformly in the solar surface (voids and clumps) Are they created by a scale free solar dynamo? Are they of different origin but all are dominated by surface turbulence? However The quiet Sun seems to be the same magnetism everywhere in the Sun The changes with the solar cycle seem to be not very large, if existent Faurobert et al. 2001, Sánchez Almeida 2003, Shchukina & Trujillo Bueno 2003, Harvey 2010

18 When interpreting inferred quantities, we usually disagree The most recent controversy is related to the inclination distribution of magnetic fields Orozco Suárez et al. 2012, ApJ, 751, 2 Martínez González et al. 2008, A&A, 477, 953 See also Stenflo 2013, A&A 555, 132

19 When interpreting inferred quantities, we usually disagree The most recent controversy is related to the inclination distribution of magnetic fields Orozco Suárez et al. 2012, ApJ, 751, 2 Orozco Suárez & Katsukawa 2012, ApJ, 746, 182 See also Stenflo 2013, A&A 555, 132

20 When interpreting inferred quantities, we usually disagree Different modeling (not different observational techniques!!) leads to huge differences on the magnetic energy content: One magnetic element: hg (200 G) fields occupying 10 20% Khomenko et al. (2003), Martínez González et al. (2008), Orozco Suárez et al. (2008)

21 When interpreting inferred quantities, we usually disagree Different modeling (not different observational techniques!!) leads to huge differences on the magnetic energy content: One magnetic element: hg (200 G) fields occupying 10 20% Khomenko et al. (2003), Martínez González et al. (2008), Orozco Suárez et al. (2008)

22 When interpreting inferred quantities, we usually disagree Different modeling (not different observational techniques!!) leads to huge differences on the magnetic energy content: One magnetic element: hg (200 G) fields occupying 10 20% Khomenko et al. (2003), Lopez Ariste et al. 2006, Martínez González et al. (2008), Orozco Suárez et al. (2008) MISMA: hg and kg fields coexisting Sánchez Almeida (2002), Domínguez Cerdeña et al. (2005), Viticchiè et al. (2010) Microturbulent approximation: G filling 100% Faurobert et al. (2001), Trujillo Bueno et al. (2004)

23 When interpreting inferred quantities, we usually disagree WHY??!! Low signal to noise data Stenflo 2010, A&A, 517, 37 See also Bellot Rubio et al. 2003, Asensio Ramos 2009, Borrero & Kobel 2012

24 When interpreting inferred quantities, we usually disagree WHY??!! Low signal to noise data Stenflo 2010, A&A, 517, 37 See also Bellot Rubio et al. 2003, Asensio Ramos 2009, Borrero & Kobel 2012 Degeneracies in the inverse problem Martínez González et al. 2006, Asensio Ramos et al. 2008

25 When interpreting inferred quantities, we usually disagree BAYESIAN INFERENCE a 1,, Δa 1 a 2,, Δa 2 a 3,, Δa 3 a 4,, Δa 4 a 5,, Δa 5 a n,, Δa n

26 When interpreting inferred quantities, we usually disagree BAYESIAN INFERENCE b 1,, Δb 1 b 2,, Δb 2 a 1,, Δa 1 a 2,, Δa 2 a 3,, Δa 3 a 4,, Δa 4 a 5,, Δa 5 a n,, Δa n b 3,, Δb 3 a 4,, Δa 4 b 5,, Δb 5 b n,, Δb n a i b i

27 When interpreting inferred quantities, we usually disagree BAYESIAN INFERENCE Hierarchical approach Asensio Ramos & Martínez González 2014, A&A, in press

28 Muchas gracias!

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