## Friday, 26 April 2019

### XXXI Canary Islands Winter School: Computational Fluid Dynamics in Astrophysics

Registration is now open for the XXXI Canary Islands Winter School of Astrophysics, which will be held this year in La Laguna, Tenerife, Spain from 19-28 November, on the topic of "Computational Fluid Dynamics in Astrophysics". Confirmed invited lecturers are

Fernando Moreno-Insertis (Fluid dynamics, conservation laws and waves)
Ake Nordlund (Stellar and planetary formation)
Maarit Käpylä (Dynamics of solar and stellar convection zones)
Matthias Rempel (Solar Atmosphere)
Sascha Husa (General relativity and compact objects)
Stefanie Walch-Gassner (Interstellar matter)
Tom Theus (Galaxy evolution)

The school will consist of lectures, seminars tutorials, and social events including visits to the observatories in Tenerife and La Palma. It is aimed at advanced graduate students in astrophysics, as well as postdoctoral researchers, with a strong interest in the computational fluid dynamics and it applications astrophysics.

For further information and to register, please visit

http://www.iac.es/winterschool/2019/

Claudio Dalla Vecchia
Nikola Vitas
Elena Khomenko

## Wednesday, 17 October 2018

### Three-dimensional simulations of solar magneto-convection including effects of partial ionization

Astronomy & Astrophysics Volume 618 (October 2018) is just out with a figure from our paper on the cover!

The paper (Khomenko, Vitas, Collados & de Vicente 2018: A&A, ADS) describes the effects of the partial ionization on the structure, dynamics and energy balance of the low chromosphere.

## Tuesday, 4 July 2017

### How to display magnetic field lines in IDL?

It is a common problem in visualization of magnetic fields. If we assume that the potential $A$ of the magnetic field is knows, the field lines are, by definition, iso-$A$ curves. The quickest way to display them is by using the CONTOUR procedure. If the potential field is given as a 2D variable potential, then:
IDL> CONTOUR, potential, levels = levels, /xs, /ys
gives:

However, the information here is not complete without showing the actual direction of the field along the lines. It is easy to do it in IDL:

IDL> CONTOUR, potential, levels = levels, /xs, /ys
IDL> CONTOUR, potential, levels = levels, /xs, /ys, path_xy = c
IDL> FOR i = 1, N_ELEMENTS(c)/2-1, 50 DO $ ARROW, c[0, i-1], c[1, i-1], c[0, i], c[1, i], /norm, /solid, hsize = 5  produces: It is much better now, but the arrow heads from different field lines make it crowded. If we are interested in individual field lines, we can add color to this: ## Tuesday, 11 April 2017 ### Deep-learning about horizontal velocities at the solar surface The velocity fields are of great importance for understanding dynamics and structure of the solar atmosphere. The line of sight velocities are coded in the wavelength shifts of the spectral lines, thanks to the Doppler effect, and relatively easy to measure. On the other hand, the orthogonal ("horizontal") components of the velocity vector are impossible to measure directly. The most popular method for estimating the horizontal velocities is so-called local correlation tracking (LCT, November & Simon, 1988). It is based on comparing successive images of the solar surface in the continuum light and transforming their differences into information about the horizontal fields. However, the LCT algorithm suffers from several limitations. In a paper by Andres Asensio Ramos and Iker S. Requerey (with a small contribution from my side) accepted by A&A and published on Arxiv some weeks ago (2017arXiv170305128A) this problem is tackled by the deep-learning approach. A deep fully convolutional neural network is trained on synthetic observations from 3D MHD simulations of the solar photosphere and then applied to the real observation with the IMaX instrument on board the SUNRISE balloon (Martinez Pillet et al, 2011; Solanki, 2010). The method is validated using simulation snapshots of the quiet sun produced with the MANCHA code that I have been developing in the last couple of years. ## Monday, 20 March 2017 ### K-means clustering The problem of clustering is a rather general one: If one has$m$observations or measurements in$n$dimensional space, how to identify$k$clusters (classes, groups, types) of measurements and their centroids (representatives)? The k-means method is extremely simple, rather robust and widely used in it numerous variants. It is essentially very similar (but not identical) to Lloyd's algorithm (aka Voronoi relaxation or interpolation used in computer sciences). k-means Let's use the following indices:$i$counts measurements,$i \in [0, m-1]$;$j$counts dimensions,$j \in [0, n-1]$;$l$counts clusters,$l \in [0, k-1]$. Each measurement in$n$-dimensional space is represented by a vector$x_i = \{x_{i, 0}, \dots x_{i, n-1}\}$, where index$i$is counting different measurements ($i = 0, \dots, m-1$). The algorithm can be summarized as: 1. Choose randomly$k$measurements as initial cluster centers:$c_0, ..., c_{k-1}$. Obviously, each of the clusters is also$n$-dimensional vector. 2. Compute Euclidean distance$D_{i, l}$between every measurement$x_i$and every cluster center$c_l$: $$D_{i, l} = \sqrt{\sum_{j=0}^{n-1} (x_{i, j} - c_{l, j})^2}.$$ 3. Assign every measurement$x_i$to the cluster represented by the closest cluster center$c_l\$.

4. Now compute new cluster centers by simply averaging all the measurements in each cluster.

5. Go back to 2. and keep iterating until none of the measurements changes its cluster in two successive iterations.

This procedure is initiated randomly and the result will be slightly different in every run. The result of clustering (and the actual number of necessary iteration) significantly depends on the initial choice of cluster centers. The easiest way to improve the algorithm is to improve the initial choice, i.e. to alter only the step 1. and then to iterate as before. There are to simple alternatives for the initialization.

## Wednesday, 1 February 2017

### First observation of linear polarization in the forbidden [OI] 630.03 nm line

In a new paper (de Wijn, Socas-Navarro & Vitas, 2017, ApJ, 836, 29D) we present the first results of our observations of a sunspot and an active region using the SP/SOT instrument on board the Hinode satellite. The novelty in our observation is a trick that we used to double the standard wavelength range observed by the instrument. Thanks to that, we were able to see the sun not only in the two iron lines at 630.2 nm, but also in four other lines. One of those is particularly interesting: the forbidden ground-based line of neutral oxygen ([OI] 630.03 nm). It is one of only few oxygen lines in the solar spectrum and probably the best diagnostics of the solar oxygen abundance. For the first time ever we observed the linear polarization in this line! As an M2 (magnetic dipole) transition, it is predicted by the theory (Landi degl'Innocenti and Landi, 2004, Section 6.8) that this line produces the linear polarization signal with the opposite sign to the lines produced by E2 transitions. It is also the first time that linear polarization in M2 and nearby E2 lines is measured simultaneously, so that the flip in sign is obvious (see the left-most spectral line in the red circle in the Figure; in linear polarization it has "W" shape, while all other lines in the wavelength range have "M" shapes). This result may bring new light to the ongoing debate on the solar oxygen crisis.

More details of this unique observation will appear soon in a follow-up publication.

## Wednesday, 30 November 2016

### 1D Solar Atmosphere Models in IDL: Penumbra by Ding & Fang (1989)

Plane-parallel atmosphere in hydrostatic equilibrium published by Ding & Fang (1989, "A semi-empirical model of sunspots penumbra", 1989A&A...225..204D). Statistical equilibrium for hydrogen model-atom with 12 levels plus continuum. The model is produced by fitting observations of penumbra in  2 lines of H and 5 lines of Ca. The observations were carried out on McMath telescope at Kitt Peak National Observatory. The observed sunspot was small, rounded and close to the disk center. The field strength in the umbra was around 1.25 kG and 560 G in the penumbra.

It is interesting to note their Fig.2 (see it below). In the deep photosphere, the temperature in this model is similar to the temperature in the model of Yun et al. (1981). However, between the optical depths -3 and -4 it becomes close to the VALC model (Vernazza et al, 1981).