Studying the internal structure of exoplanet-host stars compared to that of similar stars without detected planets is particularly important for the understanding of planetary formation. The observed average overmetallicity of stars with planets is an interesting point in that respect. In this framework, asteroseismic studies represent an excellent tool to determine the structural differences between stars with and without detected planets. It also leads to more precise values of the stellar parameters like mass, gravity, effective temperature, than those obtained from spectroscopy alone. Interestingly enough, the detection of stellar oscillations is obtained with the same instruments as used for the discovery of exoplanets, both from the ground and from space. The time scales however are very different, as the oscillations of solar type stars have periods around five to ten minutes, while the exoplanets orbits may go from a few days up to many years. Here I discuss the asteroseismology of exoplanet-host stars, with a few examples.

This paper discusses numerical simulations performed in order tobetter understand the dynamics of various physical processes present in theradiative regions of stars. Those processes includesemi-convection, Eddington-Sweet meridional circulationand anisotropic turbulence. The impact of some of those results onevolutionary models is also discussed.

Hot core chemistry, characterized by the evaporation of icy mantle molecules from dust grains and subsequent gas-phase chemistry, seems ubiquitous in hot, dense clouds. Hot core molecules have been observed, not only in high-mass star-forming regions, but also in protoplanetary disks, shocks in young stellar outflows, and so on. Here, we study grain-surface chemistry and chemistry in hot gas in disks and outflows. Our results suggest that observations of molecular lines by the forthcoming ALMA and other facilities will give us information on, for example, grain-surface chemistry in the outer disk, turbulent mixing in the inner disk, and the physical and chemical conditions at the launching points of outflows.

Active hot stars are hot stars (Teff ≥ 8000 K) exhibiting emission lines (namely hydrogen lines) and IR excess which both originate in a circumstellar environment. In this paper we present in details the SIMECA (SImulation pour Etoiles Chaudes Actives) code which is the only code freely available to model the gaseous environment of active hot stars. It computes line profiles, Spectral Energy Distributions (SED) and intensity maps, which can be directly compared to high angular resolution observations.

Carbonaceous cosmic dust is mainly observed through infrared spectroscopy either in absorption or in emission. Laboratory soot analogues of this interstellar or circumstellar dust were produced in fuel-rich, low-pressure, premixed and flat, flames. The particles were investigated by infrared absorption spectroscopy in the 2–15 μm spectral region. The details of the spectral features shed some light on the structure of the material and enable the study of its life cycle. In particular, the 8 μm band position is tentatively attributed to defects at the edge or in the polyaromatic units of the materials, revealing these structural changes in astrophysical dust.

We briefly outline the plans for scientific activities with the International Robotic Antarctic Infrared Telescope (IRAIT), recently mounted at Dome C. We summarize a few fields where infrared observations with the IRAIT telescope can be effective and we focus on a key project for the Commissioning Phase, namely the determination of the luminosity and of evolutionary parameters for evolved Long-Period Variables (LPVs).

Chromospheric evaporation suggests the mass upflows from chromosphere to corona after the electron heating at the chromosphere during the solar flares. It takes place at the rising phase, and has a typical timescale about 100 s and a typical speed about 300–400 km s-1. Such characteristics are well observed as the blueshift at the spectral lines. By the way, the facts of the high-frequency cutoff negatively drifting on the radio dynamic spectra and the hard X-ray footpoint source motions along the loop legs are also thought to be the signatures of the chromosphere evaporation. In this paper, we show the observational evidences of the chromospheric evaporation at radio, EUV and X-ray emissions.

Supersymmetry (SUSY) is a theoretically attractive scenario for physics beyond the Standard Model which provides a suitable Dark Matter candidate in case R-parity is conserved. If SUSY is realized at the TeV scale, as favored by several arguments, it will be accessible at the Large Hadron Collider (LHC) at CERN within the first few years of data taking. We present search strategies for generic SUSY models with R-parity conservation with the ATLAS detector at the LHC. These inclusive search strategies are based on signatures including missing transverse momentum from undetected neutralinos, multiple jets and leptons or b and tau jets. We show the corresponding discovery reach for the first fb-1 of ATLAS data and discuss possible measurements needed to extract the masses of SUSY particles including the undetected neutralino.

The large galaxies in the Local Group, as all disk galaxies, havediverse stellar populations. A better understanding of thesedifferences, and a physical understanding of the causes, requires moredetailed study of the older populations. This presents a significantchallenge to GAIA but the scientific returns are also significant.

We study the evolution of the emerging and eruptive Active Region (AR) 10930 for which the coronal magnetic field is reconstructed as a nonlinear force-free field along with vector magnetograms obtained from Hinode/SOT/SP data. We show that the AR evolves quasi-statically during several days through a sequence of equilibria until the time of the eruption. In addition this sequence emphasizes the formation and expansion of a coronal Twisted Flux Rope (TFR) which is related to other observed coronal structures. On the other hand, the pre-eruptive and post-eruptive magnetic configurations show that the pre-eruptive TFR plays a crucial role during the eruption.

We have searched for magnetic fields in several early B-type stars:βCephei, Slowly Pulsating B (SPB) and in particular Be stars. We recallthe properties of these stars and highlight the problem of the Be phenomenon. Wediscuss two clues towards understanding this phenomenon in terms of pulsations andmagnetic fields. We summarize results from spectropolarimetric observationsobtained at the Pic du Midi (France) and highlight the results for the Be starω Ori and the β Cep star V2052 Oph.

Atomic diffusion has been suggested to play a significant role in a large variety of CP stars to reproduce observations. In this paper I will briefly present the physics included in the self-consistent models that include atomic diffusion and radiative accelerations. I will discuss their effect on the evolution and on the internal structure of Pop I and Pop II stars, as well as the effect on the predicted surface abundances. I will also present the effect on cluster age determination.

We present the radial velocity (RV) distribution of Carina dSph, obtained using low-, medium- and high-resolution spectroscopic data collected with FORS2 and GIRAFFE at the VLT. We found that regions where the mean RV is smaller the dispersion is also smaller, and the RV distribution is sharper (i.e. the kurtosis attains larger values). The mean RV, when moving to lower Galactic latitude, decreases by ∼ 5kms−1, attains a well defined minimum outside the galaxy center, and a constant value at larger distances. The RV gradient appears to be in the direction of the Carina proper motion. However, this parameter is affected by large uncertainties to reach a firm conclusion. These findings are probably reminiscent of a substructure with transition properties, already detected in dwarf ellipticals, and call for independent confirmations.

The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) has recently conducted an extragalactic submillimetric survey of the Chandra Deep Field South region of unprecedented size, depth, and angular resolution in three wavebands centered at 250, 350, and 500 µm. BLAST wavelengths are chosen to study the Cosmic Infrared Background near its peak at 200 µm. We find that most of the CIB at these wavelengths is contributed by galaxies detected at 24 µm by the MIPS instrument on Spitzer, and that the source counts distribution shows a population with strongly evolving density and luminosity. These results anticipate what can be expected from the surveys that will be conducted with the SPIRE instrument on the Herschel space observatory.

We discuss in this paper the new science perspectives that a near infrared (NIR) spectropolarimeter installed on a 4 m class telescope at Dome C in Antartica would offer to the astrophysics community worldwide, in very diverse research fields such as stellar formation, extra solar planets, stellar magnetism and activity, asteroseismology, circumstellar environments, interstellar medium, galactic and extragalactic physics. We also propose an instrument concept with estimated performances, as well as an example 2-step scenario for the construction of this instrument.

In this lecture, we briefly present the main models currently proposed to describe the collapse of prestellar dense cores and the formation of young Class 0 protostars. An empirical evolutionary sequence for the formation of low-mass stars is described. Then, the typical properties of Class 0 protostars are reviewed and the question of their structure at small scales is adressed through the question of circumstellar disks.

Very high energy gamma-ray astronomy is now bringing an invaluable contributionto the understanding of violent phenomena in the Universe, as well as the searchfor exotic physics such as indirect detection of dark matter or a test ofLorentz invariance violation. The current Imaging Arrays of Cherenkov Telescopes(IACT) show that this technique is mature. In Europe, the community is gatheringaround the Cherenkov Telescope Array consortium, to design and build the next generationground-based array. It should reach an order of magnitude in sensitivity in awide energy band, ranging from 10 GeV to more than 100 TeV. This goal can beachieved with an array of 50–100 telescopes of various sizes at variousspacings. With about 2000 channels per camera, a specific effort has to be madeto design front-end electronics with a lower cost and better performances.A gain in cost and performances can be obtained by maximising the integration of thefront-end electronics in an ASIC. The amplifiers, analogue memories,digitization and first level buffering can be embedded in the same component.We present here the NECTAr project aiming at building a demonstrator element ofa generic camera built around this component.

We use numerical simulations to study the dynamical effect of substructure inCold Dark Matter (CDM) halos on stellar galactic disks. Substructure halos withmasses, densities and orbits derived from high-resolution cosmological CDMsimulations play only a minor dynamical role in the heating of the disk overseveral Gyrs. This is because the orbits of dark satellites in CDM halos seldomtake them near the disk, where their tidal effects are greatest. The mostnoticeable effects of substructure in our simulation may be traced to the mostmassive sub-halo and include: (i) the forcing of short-lived stellar warps in thedisk as a result of tidal shocks that arise during each pericentric passage, and(ii) the tilting of the disk caused by the orbital decay of the satellite. These results imply that substructure might not preclude virialized CDM halos from being acceptable hosts of thin stellar disks like that of the Milky Way, and that the ubiquity of minor stellar warps may be associated with the recurrent tidal influence on the disk of the most massive substructure halos.

We present a Monte Carlo (MC) radiative transfer code for complex three dimensional dust distributions and include transiently heated PAH. The correctness of the code is confirmed by comparison with benchmark results. The method makes use of the parallelization capabilities of modern vectorized computing units like graphic cards. The computational speed grows linearly with the number of graphical processing units (GPU). On a conventional desktop PC, our code is up to a factor 100 faster when compared to other MC algorithms. As an example, we compute the dust emission of proto-planetary disks. We simulate how a mid-IR instrument mounted at a future 42 m ELT will detect such disks. Two cases are distinguished: a homogeneous disk and a disk with an outward migrating planet, producing a gap and a spiral density wave. We find that the resulting mid-IR spectra of both disks are almost identical. However, they can be distinguished at those wavelengths by coronographic, dual-band imaging. Finally, the emission of PAHs exposed to different radiation fields is computed. We demonstrate that PAH emission depends not only on the strength but also strongly on the hardness of the radiation, a fact which has often been neglected in previous models. We find that hard photons (>20  eV) easily dissociate all PAHs in the disks of T Tauri stars. To explain the low, but not negligible detection rate (<10%) of PAHs in T Tau disks, we suggest that turbulent motions act as a possible path for PAH survival.

An introduction to R is proposed. This pratical session is an excerpt from practical exercises proposed by A. Dalalyan at EPNC (see http://certis.enpc.fr/∼dalalyan/Download/TP_ENPC_1.pdf). Datas are also extracted from a practical session proposed by hydrologic data from Amazonia proposed by D. Chessel A.B. Dufour in Lyon 1 (website indicated in the text below) and from other practical exercises proposed by A. Dalalyan at ENPC (same address as above but ended by /TP_ENPC_4.pdf).