NASA Technical Reports Server NTRS 20150004438: Multiple Absorption Components in the Post-Periastron He I P Cygni Absorption Troughs of Eta CarinaeReport as inadecuate



 NASA Technical Reports Server NTRS 20150004438: Multiple Absorption Components in the Post-Periastron He I P Cygni Absorption Troughs of Eta Carinae


NASA Technical Reports Server NTRS 20150004438: Multiple Absorption Components in the Post-Periastron He I P Cygni Absorption Troughs of Eta Carinae - Download this document for free, or read online. Document in PDF available to download.

Download or read this book online for free in PDF: NASA Technical Reports Server NTRS 20150004438: Multiple Absorption Components in the Post-Periastron He I P Cygni Absorption Troughs of Eta Carinae
We have obtained more than 100 high spectral resolution R approx. 90,000 spectra of the massive binary star eta Carinae since 2012 in an effort to continue our orbital and long-term echelle monitoring of this extreme binary Richardson et al. 2010, AJ, 139, 1534 with the CHIRON spectrograph on the CTIO 1.5 m telescope Tokovinin et al. 2013, PASP, 125, 1336 in the 4550-7500A region. We increased our monitoring efforts and observation frequency as the periastron event of 2014 has approached, and resumed observations in October. We note that since mid-October, we have observed unusual multiple absorption components in the P Cygni troughs of the He I lines 4714, 5876, 6678, and 7065; 4921 and 5015 are blended with Fe II. In particular, we note that these components extend to -700 km-s, well beyond the terminal wind speed of the primary. These absorptions are likely related to clumps and turbulence in the wind-wind collision region and bow shock, as suggested by the high-velocity absorption observed by Groh et al. 2010, AandA, 519, 9 in the He I 10830A transition and our pre-periastron observations Richardson et al. 2014, ATel #6336. In these cases, we suspect that we look along an arm of the shock cone and that we see a fast absorption change from the other collision region shortly after periastron. Further, high spectral resolution data are highly encouraged, especially for resolving powers greater than 50,000. These observations were obtained with the CTIO 1.5 m telescope, operated by the SMARTS Consortium, and were obtained through both SMARTS and NOAO programs 2012A-0216, 2012B-0194, and 2013b-0328. We thank Emily MacPherson Yale for her efforts in scheduling the observations that we have and will obtain in the coming weeks and months.



Author: NASA Technical Reports Server (NTRS)

Source: https://archive.org/



DOWNLOAD PDF




Related documents