1. Towards developing new Italian IVOA simulation data services:
INAF Science Archives and the Big Data Challenge
17-18 June 2019, Rome
Towards developing new Italian IVOA simulation data services:
I. Exoplanet case- ARTECS data service-archive of terrestrial-type climate simulations
II. MHD instabilities simulations at planetary magnetospheres
III. MATISSE web-tool function integrations: real-time computations and visualization of aerodynamic coefficients
Stavro L. Ivanovski1,
Marco Molinaro1 , Giuseppe Murante1, Cristina Knapic1, Giovanni Vladilo1
1INAF- Ossservatorio Astronomico di Trieste (OATS), Roma, 00133, Italy
Milillo A.2, Kartalev M.3, Massetti S.2, Orsini S.2, Sordini R.2, Mura A.2, Mangano V.2, De Angelis E.2, Rispoli R.2, Lazzarotto F.2, Aronica A.2, Kazakov A.2
2INAF - Institute for Space Astrophysics and Planetology, Rome
3Geospace Consult Ltd, Institute of Mechanics, Bulgarian Academy of Sciences, Sofia, Bulgaria.
A. Zinzi 4,5, M.T. Capria 2,4 , V. Zakharov 2 M. Giardino 4, S. Erard 6, A. Longobardo 2, S. Fonte 2, L. A. Antonelli 4,5, V. Della Corte 2,7, A. Rotundi 2,7
4 ASI-SSDC, via del Politecnico snc, I Rome, Italy,
5 INAF-OAR, via di Frascati 33, Monte Porzio Catone (RM), Italy,
6 LESIA, Observatoire de Paris/CNRS/Universite ́ Pierre et Marie Curie/Universite ́ Paris-Diderot, F Meudon, France
7 Università degli Studi di Napoli “Parthenope”– Centro Direzionale Isola C4, Napoli, Italy,
Stavro L.. Ivanovski

2. Context and background: VESPA and Italian IVOA data services Small Bodies
VESPA (Virtual European Solar and Planetary Access), within the H2020 Europlanet project, developed such an infrastructure and deals with implementation of new data services (Erard et al., 2018,PSS).
For simulations that do not produce significant data volume, such approach is feasible, and can even accommodate simulation results of different scenarios or inputs.
Stavro L.. Ivanovski

3. Context and background: VESPA and Italian IVOA data services in Small Bodies
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
Stavro L.. Ivanovski

4. Context and background: VESPA and Italian IVOA data services in Small Bodies
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
Stavro L.. Ivanovski

5. I. Exoplanet case- ARTECS data service-archive of terrestrial-type climate simulations
Stavro L.. Ivanovski

6. I. Exoplanet case- ARTECS data service-archive of terrestrial-type climate simulations
Stavro L.. Ivanovski

7. MHD Instabilities and Mercury Magnetopause
II. MHD instabilities simulations at planetary magnetospheres
Kelvin - Helmholtz instability
instability of the boundary layer separating two fluids in relative motion, generated at the boundaries of two regions (moving tangentially) with the different flow speed and/or direction and different densities.
Slavin et al. 2009, Science
Tearing mode instability -
generated at boundaries between two regions (moving tangentially ) with the different magnetic field. Typical “magnetic island” is presented in (b).
Stavro L.. Ivanovski
MHD Instabilities and Mercury Magnetopause

8. ZGSM Computational 2D domain OABC YGSM Dayside magnetopausex z O A B C
The problem is posed in a rectangular region OABC, supposed to present a cross-section of the magnetopause boundary layer
x - direction is along the velocity of the incident magnetosheath flow ;
z - direction is downward to the Earth's center (from the magnetosheath to the magnetosphere);
YGSM
ZGSM
Computational
2D domain OABC
Dayside magnetopause
view from the Sun
IMF projection on (YZ)GSM plane 8

9. DENSITY Ivanovski et al 2011
The DENSITY contours are for: t=0s; t=1s; t=3s, t=5s; t=7s; t=9s. The parameters:Re = 250; Rm=1000 Vsh= 1.0; Vmg= 0.0; zm =0.5; zd=0.5, ρsh= 5; ρmg= 0,5;Bshx= -1.0; Bmgx= 1.0Bshy= 0.0; Bmgy= 0.0; B = 0.02;  = 0.04.
DENSITY
Ivanovski et al 2011
Stavro L.. Ivanovski

10. MAGNETIC FIELD (x,z) plane Ivanovski et al 2011
The contour lines of magnetic field in (x,z)-plane are for: t=0s; t=1s; t=3s, t=5s; t=7s; t=9s. The parameters:Re = 250, Rm=1000; Vsh= 0.5; Vmg= 0.0; zm =0.5; zd=0.5, ρsh= 5; ρmg= 0,5;Bshx= -1.0; Bmgx= 1.0, Bshy= 0.0; Bmgy= 0.0; B = 0.02;  = 0.04.
MAGNETIC FIELD (x,z) plane
Stavro L.. Ivanovski
Ivanovski et al 2011

11. Different boundary conditions for VELOCITY
II. MHD instabilities simulations at planetary magnetospheres
Different boundary conditions for VELOCITY А B
Comparison between cases with different velocity on the boundary (for developed instability of the density ) for period of time t=9. In case A - Vsh=0.5, and in case B – Vsh=1.0. The parameters: Re = 250, Rm=1000; Vmg=0.0; zm =0.5, zd=0.5; ρsh=5, ρmg=0,5; Bshx= -1.0, Bmgx=1.0, Bshy=0.0, Bmgy= 0.0; B = 0.02,  =0.04.
Stavro L.. Ivanovski

12. II. MHD instabilities simulations at planetary magnetospheres
Results: MHD instabilities and magnetic reconnection with MESSENGER data
High-Shear Magnetopause reconnection 24-Nov-2011 : density, By and vorticity
When a northward planetary filed intercacts with a southward IMF: configuration highly conducive to dayside reconnection
t = 7s
t = 7s
t = 7s
Stavro L.. Ivanovski

13. Example of Data Organization:
II. MHD instabilities simulations at planetary magnetospheres
Data format
Example of Data Organization:
The code has been written in Fortran and now rewritten in C.
Metadata:
Grid_module, Initial_module, Physics_constants_module, Normal_module
Output:
ASCII file ~ 5x 40kB visualized in MATLAB
Each output file contains all physical parameters given in space.
Normalized 2D model outputs for a grid (X,Y) distance from the center of the body, B, V, rho, Vorticity in a model setup described in Ivanovski et al 2011.
Usualy three columns : X,Y, PhV.
Stavro L.. Ivanovski

14. III. MATISSE web-tool function integrations: real-time computations and visualization of aerodynamic coefficients
The large amount of planetary data acquired by planetary space missions opened room for developing processing platforms able to provide easily and efficient data access and visualization as also to enable delivery and analysis of high-level scientific data products.
We propose the implementation of a new VESPA (Virtual European Solar and Planetary Access) application using the MATISSE (Multi-purpose Advanced Tool for the Instruments of the Solar System Exploration) web-tool, to handle the computation of aerodynamic coefficients of non-spherical convex objects.
The coefficients describe the motion of these objects in rarefied gas field present in various astrophysical environments as for example protoplanetary disks and cometary coma.
Most of the state-of-the-art cometary gas-dust dynamical models use spherical particles. The new application will provide the aerodynamic coefficients for convex objects and “averaged” ones ready as inputs to the spherical dust codes approximating realistic convex object shapes.
Stavro L.. Ivanovski

15. Calculation of Aerodynamic Coefficients in Rarefied Gas Dynamics for convex objects
where  Vr = Vg− Vd is the gas-grain (center of mass) relative velociity vector, ρ is the gas mass density, ρVr2/2 is the dynamic pressure, and S is a shape-dependent characteristic cross-section.
Similarly, for the torque  Ma one may define the dimensionless aerodynamic torque coefficient CM  
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
where A is a shape-dependent characteristic linear dimension of the grain. 
Stavro L.. Ivanovski
Ivanovski et al. 2017, Icarus

16. Calculation of Aerodynamic Coefficients in Rarefied Gas Dynamics for convex objects
Drag coefficient, lift-to-drag ratio and torque coefficient as functions of α for ellipsoids of the same volume with a/b = 2 (left) and a/b = 0.5 (right) with Td/Tg = 1 and 10. Top panels: CD (a/b = 2; 0.5) and CL/CD (a/b = 2). Bottom panels: CL/CD (a/b = 0.5) and CM (a/b = 2; 0.5). Curves with similar appearance on different panels refer to the parameter values indicated on top of the upper left panel. The big colored dots in the top left panel indicate the (alpha-independent) values for a sphere of the same volume(a/b = 1): the filled circles for Td/Tg = 1 and the non-filled for Td/Tg = 10.
Ivanovski et al. 2017, Icarus

17. MATISSE
MATISSE (Multi-purpose Advanced Tool for the Instruments of the Solar System Exploration) is a web-tool developed for the 3D visualization of small bodies shape models, single observations or real-time computed high-order products.
Zinzi et al Astronomy &Computing
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
MATISSE connects with VESPA through a Simple Application Messaging Protocol (SAMP). We discuss the procedure that enables to exchange the aerodynamic simulation results between MATISSE and VESPA interfaces.
We present the design and the implementation of a new scientific real-time application facilitating the astrophysical community to deal with the computation of irregular objects motion in a rarefied gas flow.
Stavro L.. Ivanovski

18. Real-time computation and visualization of aerodynamic coefficients
The implementation of the aerodynamic application is based on the approach by Ivanovski et al. (2017) and provide the following functionality:
choice and visualization of irregular object shape;
choice and visualization of the Euler solution of ideal gas flow;
real-time computation (if not available as precomputed) of the aerodynamic coefficients;
plots of the aerodynamic coefficients vs the dynamical parameters of the convex objects.
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
Stavro L.. Ivanovski

19. Real-time computation and visualization of aerodynamic coefficients(2a/2)
Stavro L.. Ivanovski

20. Real-time computation and visualization of aerodynamic coefficients(2b/2)
Stavro L.. Ivanovski
Ivanovski et al. 2019, in prep.

21. Real-time computation and visualization of aerodynamic coefficients
Stavro L.. Ivanovski
Ivanovski et al. 2019, in prep.

22. Current activities
The implementation of the aerodynamic application is based on the approach by Ivanovski et al. (2017) and provide the following functionality:
choice and visualization of irregular object shape and choice and visualization of the Euler solution of ideal gas flow;
real-time computation (if not available as precomputed) of the aerodynamic coefficients;
plots of the aerodynamic coefficients vs the dynamical parameters of the convex objects.
design and implementation of IVOA data service with aerodynamic coefficients.
How the transport of momentum and plasma occurs across a boundary remains a question of outstanding scientific interest.
Stavro L.. Ivanovski

23. Future Projects in Planetary IVOA data services in Italy
Towards developing new Italian IVOA simulation data services:
Future Projects in Planetary IVOA data services in Italy
Europlanet 2024 RI
OATs and the hosted INAF IA2 - One of the three regional europlanet Data Services Hub in Europe
OATs:Exoplanet case- ARTECS data service-archive of terrestrial-type climate simulation
INAF-IAPS partner in Machine Learning Solutions for data exploitation , analysis and modeling WP – the mineral identification via reflectance spectra. This topic will be faced considering some systematic laboratory datasets between mineral endmembers and their mixtures, at variable grain-sizes, training the machine to recognize specific spectral properties and their variability.
INAF – Univ. Padaova : Geological Mapping of planetray surfaces
). The Centre has been created with long-term goal to implement a new strategy for preserving and providing access to the Astrophysical data heritage by coordinating different national initiatives. A particular effort was made to ensure a close interaction with a number of existing national and international projects aimed at developing and implementing advanced data mining and visualization tools, in particular in the context of the EURO-VO activities. IA2 services include the management of data archives of TNG and LBT, the support to personal databases associated to large projects (such as the UVES Large Program and the Architecture and Tomography of Galaxy Clusters project), and the development of the Italian Theoretical Virtual Observatory (ITVO). A number of researchers are involved in Virtual Observatory activities within the International Virtual Observatory Alliance (IVOA) and the Euro-VO collaborations. The current theoretical archive hosted at Trieste consists of outcomes of a set of cosmological simulations run with the GADGET and ENZO codes. Multi-levels of metadata are available including a large catalogue of Chandra synthetic observations of simulated galaxy clusters. IA2 infrastructure provides INAF coordination of all the major Italian participated ground based Telescopes and some ESO Surveys advanced products as well as theoretic simulations Archives. It is distributed in some of the INAF Institute sites like Trieste Astronomical Observatory (main site), Istituto di Radio Astronomia in Bologna, Catania Astrophysical Observatory, Asiago Astronomical Observatory, Sardinia Radio Telescope, Telescopio Nazionale Galileo as well as Large Binocular Telescope Observatory in Arizona, Max Plank Institute in Heidelberg and Ohio State University in Ohio. It supports Virtual Observatory (VO) compliant resource and service development and deployment. In Trieste, it is composed by a multi layer infrastructure for the data persistence and preservation having a SAN infrastructure for the data publication via web portals and services and a persistence infrastructure for long term preservation (TAPE library). The complex capacity of about 1 PB in expansion to 2 PB in the incoming months and to 13.5 PB in the near future. The IA2 infrastructure is connected to the GARR 10GB backbone. The archiving system is supported by redundant high performance physical servers, virtualized to host several services. The IA2 developed services main capability is the high configuration and scalability of the system in a distributed environment. The IA2 infrastructure supported also an internally developed tool (VODance) to publish in a VO compliant manner the archives. The services are now deployed through a set of applications that allow for a better distributed infrastructure. Cone Searches and SIAP-based services serve various catalogues, while TAP services, deployed through the TAPlib Java solution, support the publication of all the Telescope Archives. Moreover, a PostgreSQL plus PgSphere form the basis of the relational database backend of the services support geometric discovery.
Stavro L.. Ivanovski