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Warm and hot circumstellar gas in V1647 Ori during the 2008-2009 outburst

Carmona, A. ; Audard, M. ; van den Ancker, M. ; van der Plas, G. ; Goto, M. ; Fedele, D.

In: Proceedings of the International Astronomical Union, 2009, vol. 5, no. H15, p. 751-751

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    Titel
    • Warm and hot circumstellar gas in V1647 Ori during the 2008-2009 outburst
    Autor
    • Carmona, A.. ISDC & Geneva Observatory, ch. d'Ecogia 16, 1290 Versoix, Switzerland email: andres.carmona@unige.ch
    • Audard, M.. ISDC & Geneva Observatory, ch. d'Ecogia 16, 1290 Versoix, Switzerland email: andres.carmona@unige.ch
    • van den Ancker, M.. European Southern Observatory, Karl Schwarzschild Str 2, D-85748 Garching, Germany
    • van der Plas, G.. European Southern Observatory, Karl Schwarzschild Str 2, D-85748 Garching, Germany
    • Goto, M.. Max-Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
    • Fedele, D.. Max-Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
    Dokumententyp
    • Postprint
    Sprache
    • Englisch
    Veröffentlicht in
    • Proceedings of the International Astronomical Union, 2009, vol. 5, no. H15, p. 751-751. Cambridge University Press
    Andere elektronische Ausgabe
    OAI-PMH-ID
    • oai:doc.rero.ch:302354
    Summary
    The pre-main sequence star V1647 Ori started a new outburst in August 2008. From October 2008 to February 2009 we monitored V1647 Ori, obtaining quasi-simultaneous VLT-CRIRES near-IR spectroscopy, VLT-VISIR mid-IR spectroscopy and VLT-FORS2 optical spectroscopy. We studied the evolution of H2 and CO emission from hot and warm gas and Hα and forbidden line-emission during the initial outburst phase of V1647 Ori. Hα is observed in emission displaying P-Cygni profiles with blue-shifted absorption up to -700 km/s, suggesting the presence of a high velocity wind (Fig. 1a). [OI] emission at 6300 Å is observed displaying a blue-shifted emission shoulder, indicating the presence of material moving away from the star (Fig. 1b). We detect H2 1-0 S(1) and CO (P4 to P14 and P30-P38) ro-vibrational lines centered at the velocity of the star at all epochs (Fig. 1c & d). This strongly suggests that the H2 and CO emission originates from a disk and not from a warm outflow. The H2 1-0 S(0) and 2-1 S(1) ro-vibrational lines at 2.22 and 2.24 μm and the pure-rotational H2 0-0 S(1) and 0-0 S(2) lines at 17 and 12 μm were not detected in our spectra. Changes in the Hα and [OI] profiles and the H2 and CO emission observed do not correlate. We modeled the H2 and CO line profiles assuming emission from a flat disk in keplerian rotation with line intensity decreasing with radius (I ~ I0(R/Rmin)−α). We found that the disk of V1647 Ori is observed nearly face-on and that the line emission is produced within a fraction of an AU of the star (Fig. 1d)