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This is the written account of the second of two panel discussions, on Reconciling observations and modeling of star formation at high redshifts. The chair of the panel was Pavel Kroupa, and panel members were Marc Balcells, John Beckman, Christopher Conselice, and Joseph Silk. After a short introduction by each of the panelists, panel and audience

This is the written account of the first of two panel discussions, on Star formation in galaxies: how do we continue? The chair of the panel was Phil James, and panel members were John Beckman, Torsten Böker, Daniela Calzetti, Angeles Díaz, and Rob Kennicutt. The panel and audience discussed the following four questions: 1) What are the most

In this work we investigate p-mode power variation with solar atmosphere. To this aim, we use THÉMIS observations of the Na D1 (λ5896 Å) and K (λ7699 Å) spectral lines. While the formation heights of the K spectral line are essentially located in the photospheric layer, the formation heights of the Na D1 line span a much wider region: from

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Using 21 cm observations of Complex H with the Green Bank Radio Telescope, we have derived its LSR velocity of ˜ 200 km s-1 and an H I mass of 7.5× 107 M&sun;. This gives useful support to the scenario in which the Galactic disk is being built up by the continual accretion of clouds of this type from the intracluster medium of the Local Group