scholarly journals New insights into the WR nebula M1-67 with SITELLE

2020 ◽  
Author(s):  
Marcel Sévigny ◽  
Nicole St-Louis ◽  
Laurent Drissen ◽  
Thomas Martin
Keyword(s):  
Fourier Transform ◽  
Emission Line ◽  
Electron Density ◽  
High Velocity ◽  
Point Of View ◽  
Bow Shock ◽  
Fourier Transform Spectrometer ◽  
Chemical Abundance ◽  
Electron Density And Temperature ◽  
Rayet Star

Abstract We present a detailed study of M1-67, a well-known nebula around the population I Wolf-Rayet star WR 124 (WNh 8), based on datacubes obtained with the imaging Fourier transform spectrometer SITELLE at the Canada-France-Hawaii Telescope (CFHT). This allowed us to reconstruct detailed emission-line ratio maps that highlight clear orthogonal features from a chemical abundance point of view, a complete extinction map, as well as the electron density and temperature structures. In addition to this information, velocity maps were obtained shedding light on the bow shock structure due to the high velocity of WR124, qualified as a runaway star, which is about +190 km s−1 relative to the local ISM. Interaction between the latter structure and spherical and non-spherical outburst could explain the global morphology of M1-67.

THEORETICAL ELECTRON DENSITY AND TEMPERATURE SENSITIVE EMISSION LINE RATIOS FOR HELIUM-LIKE Si XIII COMPARED TO DITE TOKAMAK OBSERVATIONS

1989 ◽  
Vol 50 (C1) ◽  
pp. C1-559-C1-564
Author(s):  
F. P. KEENAN ◽  
R. BARNSLEY ◽  
J. DUNN ◽  
K. D. EVANS ◽  
S. M. McCANN ◽  
...  
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Temperature Sensitive ◽  
Electron Density And Temperature

Electron density and temperature-sensitive x-ray-emission-line ratios for heliumlike Si xiii in the DITE tokamak

1989 ◽  
Vol 39 (8) ◽  
pp. 4092-4097 ◽  
Author(s):  
F. P. Keenan ◽  
S. M. McCann ◽  
R. Barnsley ◽  
J. Dunn ◽  
K. D. Evans ◽  
...  
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Temperature Sensitive ◽  
X Ray ◽  
Electron Density And Temperature

Quadrupole Coupling in 4-Fluoro-benzonitrile. A Microwave Fourier Transform Study

1986 ◽  
Vol 41 (5) ◽  
pp. 752-755 ◽  
Author(s):  
Olaf Böttcher ◽  
Dieter H. Sutter
Keyword(s):  
Fourier Transform ◽  
High Resolution ◽  
Electron Density ◽  
Fourier Transform Spectrometer ◽  
Nitrogen Nucleus ◽  
Quadrupole Coupling

The 14N quadrupole hfs coupling has been studied in Para-fluoro-benzonitrile using the high resolution microwave Fourier transform spectrometer constructed at Kiel University. If interpreted within a simplified MO treatment, the data show that the out-off-plane p-electron density at the Nitrogen nucleus is appearently larger than the in-plane density, contrary to the prediction of a CNDO/2 calculation.

scholarly journals Spectrophotometry of six high-excitation compact H II regions in the Magellanic Clouds

2003 ◽  
Vol 212 ◽  
pp. 753-754 ◽  
Author(s):  
Gérard Testor
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Spectral Type ◽  
Magellanic Clouds ◽  
H Ii Regions ◽  
High Excitation ◽  
Chemical Abundances ◽  
Line Intensities ◽  
Exciting Source ◽  
Electron Density And Temperature

Series of CCD long-slit spectra have been obtained in the 3600-10000 Å range, with the ESO 1.5m telescope, for the six brightest compact H ii regions in the LMC and SMC: N 11A, N 160 A1-A2 and N 88A, N 81 and N 26A-B, respectively. For each region the spectral type of its complex exciting source is given. From the emission-line intensities we have derived the gas electron density and temperature, and computed the chemical abundances of He, O, N, Ne, S, and Ar, which we compare with the ones found for other H ii regions in the Magellanic Clouds.

scholarly journals HH 34: The bow shock of a jet

1987 ◽  
Vol 122 ◽  
pp. 175-176
Author(s):  
Th. Bührke ◽  
R. Mundt
Keyword(s):  
Radial Velocity ◽  
Electron Density ◽  
High Velocity ◽  
Shock Structure ◽  
Bow Shock ◽  
Complex Velocity ◽  
Ccd Imaging ◽  
Working Surface ◽  
Lower Excitation ◽  
Hh Object

Deep CCD imaging of HH 34 in H∝ shows that the HH-object has a bow shock-like structure, of which the wings can be traced over about 1 arcmin ( pc). A knotty jet is pointing towards the apex of the bow shock structure. Long-slit spectroscopy reveals that 1) the jet has approximately a constant radial velocity and electron density. 2). The spectrum of the jet is of a much lower excitation than that of HH 34. 3) HH 34 has a complex velocity and line excitation structure. The extended bow shock is interpreted by a jet of which the working surface is propagating with high velocity (≈ 200 km/s) through a partially ionized medium.

The ISM local to the runaway star WR16

2020 ◽  
Vol 495 (1) ◽  
pp. 417-427 ◽  
Author(s):  
S Cichowolski ◽  
N U Duronea ◽  
L A Suad ◽  
E M Reynoso ◽  
A Noriega-Crespo ◽  
...  
Keyword(s):  
Molecular Structure ◽  
High Velocity ◽  
Main Sequence ◽  
Massive Stars ◽  
Bow Shock ◽  
Subsequent Stage ◽  
Infrared Band ◽  
Cold Dust ◽  
Mass Ejection ◽  
Rayet Star

ABSTRACT Massive stars leave their imprint on the interstellar medium as they radiate their energy and undergo episodes of mass ejection throughout their lives. In this paper, we analyse the case of the Wolf–Rayet star WR16 combining archival multiwavelength data with new molecular observations obtained with the Atacama Submillimeter Telescope Experiment (ASTE). Our results suggest that during the main-sequence phase, WR16 swept up the surrounding gas creating a molecular structure (which we call Component 1) which also contains very cold dust observed in the infrared band. In a subsequent stage of evolution, as an LBV, the star underwent mass eruptions that were later overrun by the fast winds of the current WR phase. The final result is the round nebula revealed by the optical and IR images, and the molecular clumps detected. We have also computed the peculiar velocity of WR16 using Gaia data and, accordingly, confirm it as a runaway star. We propose that several features observed in different wavelengths can be explained under a bow-shock scenario linked to the high velocity of WR16.

scholarly journals The Compact HII Regions N11A and N88A in the LMC and SMC

1999 ◽  
Vol 190 ◽  
pp. 132-133
Author(s):  
G. Testor ◽  
C. S. Rola ◽  
A. B. Whiting
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Spectral Type ◽  
Hii Regions ◽  
Magellanic Clouds ◽  
Chemical Abundances ◽  
Line Intensities ◽  
Exciting Star ◽  
Electron Density And Temperature ◽  
Compact Hii Regions

Several spectra have been obtained in the 3600–10000 Å range, for the HII regions N11A and N88A in the LMC and SMC, respectively. The spectral type of their exciting star was determined and from the emission-line intensities we have derived the gas electron density and temperature, and computed the chemical abundances of He, O, N, Ne, S, and Ar. These abundances are then compared with the ones found for other HII regions in the Magellanic Clouds.

White-Light Coronal Structures: Streamers and CMEs

1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
White Light ◽  
Coronal Mass Ejections ◽  
X Rays ◽  
Solar Cycles ◽  
Temperature Function ◽  
X Ray ◽  
Eclipse Observations ◽  
Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

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