1. Spatially Dependent Emergence Rate V. Abramenko

2. Outlook Compare results from the paper by Abramenko, Fisk, Yurchyshyn ApJ 641 (hereafter AFY) with that from Version 1, Version 2, Version 3, and Version 4 of the paper by Hagenaar, Schrijver, and DeRosa ( hereafter HSD-V1, HSD-V1, HSD-V1, HSD-V1) Role of the magnetic imbalance and distribution functions Impossibility to find the unique value of the emergence rate, the tendency only (effects of resolution)

3. The Rate of Emergence of Magnetic Dipoles in Coronal Holes and Outside Abramenko, Fisk, Yurchyshyn, ApJ 641, 2006. (hereafter AFY paper)

4. A number of dipoles that emerged during 24 hours inside an area of 200 x 200 Mm is taken as the Dipole Emergence Rate, m

5. HSD-V1 – V3: two CHs from the AFY data set V1 V2 V3

6. HSD-V1 – HSD-V3: two CHs from the AFY data set CH 2002/07/31 cadence CH 2003/05/30 cadence AFY: N(qs)/N(ch)= 1.73 3-5 hour HSD-V1: N(qs)/N(ch)= 1.48 5 min HSD-V2: N(qs)/N(ch) = 2.4 5.min HSD-V3: N(qs)/N(ch) = 2.6 5 min AFY: N(qs)/N(ch)= 1.19 3-5 hour HSD-V1: N(qs)/N(ch)= 1.22 5 min HSD-V2: N(qs)/N(ch)= 1.8 5 min HSD-V2: N(qs)/N(ch)= 1.6 5 min

7. HSD-V3: N(qs)/N(ch)= 2.9 HSD-V4: N(qs)/N(ch)= 0.82 Broadening of the CH boundary results in lowering of the ratio.

8. Magnetic flux imbalance, ξ Averaged number of emerged bipoles per one sample box HSD – V4

9. How the lifetime can influence the emergence rate? time QS CH 1 +1 =3 Low cadence: N(qs)=3 Low cadence: N(ch)=1 1 =1 Low cadence: N(qs)/N(ch)=3/1=3.0

10. How the lifetime can influence the emergence rate? time QS CH 1 +1 =3Low cadence: N(qs)=3 Low cadence: N(ch)=1 1 =1 Low cadence: N(qs)/N(ch)=3/1=3.0 1 +1 =3 High cadence: N(ch)=3 1 +1 =3 High cadence: N(qs)=3 High cadence: N(qs)/N(ch)=3/3=1.0 If the lifetime in CHs is predominantly shorter then the cadence improvement results in equating of registered number of emerged bipoles in CH and QS.

11. Relationship between the Lifetime and Flux Hagenaar et al. 1999 τ(l) ~ l For the stationary isotropic turbulence, the lifetime of eddies scales as: Biggest live longer Ф ~ l τ ~ Ф 2 1/2

12. Distribution of the Flux for emerged bipoles HSD – V3 QS CH PDF for QS displays a more heavy tail than the PDF of CH does. Bipoles in CHs are smaller than bipoles in QS. Therefore, their lifetime is shorter.

13. CH (open) - CH (loop) + QS Loops inside CHs are the weakest population, therefore they live shorter. The distributions are highly non-Gaussian, the averaged parameters are not suitable, the entire distribution function has to be considered. CHQS averaged

14. Ratio of cummulative distribution functions HSD – V2 QS CH

15. Conclusions For flux > 10^19Mx and for time cadence larger than 5 min, the bipole emergence rate correlates with the flux imbalance AND inside CHs it is smaller than outside. Under these restrictions, the emergence rate and flux imbalance are spatially dependent. Distribution functions of the magnetic flux content show that CHs are populated by closed loops of weaker fluxes than QS areas. This allows to suggest that the lifetime of loops in CHs is shorter than that in QS. Which might results in equating of number of emerged bipoles in CH and QS as the cadence/resolution improves. The emergence rate and flux imbalance are resolution dependent, too. Distribution functions are highly non-Gaussian. Area-averaged parameters cannot provide an appropriate representation for the expectation values of the flux content, lifetime, number of bipoles, etc. Observed distribution functions have to be applied to derive mean values of magnetic parameters.

16. Solar wind speed versus the flux imbalance in a CH