The magnetic environment of the Orion-Eridanus superbubble as revealed by <i>Planck</i>

Soler, J. D.; Bracco, A.; Pon, Andy

doi:10.1051/0004-6361/201732203

Cited by 38 publications

(42 citation statements)

References 48 publications

(58 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In regions where the magnetic field energy density is subdominant to the kinetic energy of the matter, gas dynamics will influence magnetic field morphology. This effect has been observed for Hi shells (Heiles 1998;Fosalba et al 2002;Santos et al 2011;Frisch & Dwarkadas 2017;Soler et al 2018) as well as at the edges of Hii regions (Pavel & Clemens 2012;Santos et al 2012Santos et al , 2014Planck Collaboration Int. XXXIV 2016).…”

mentioning

confidence: 80%

The Far-infrared Polarization Spectrum of ρ Ophiuchi A from HAWC+/SOFIA Observations

Santos

Chuss

Dowell

et al. 2019

ApJ

View full text Add to dashboard Cite

We report on polarimetric maps made with HAWC+/SOFIA toward ρ Oph A, the densest portion of the ρ Ophiuchi molecular complex. We employed HAWC+ bands C (89 µm) and D (154 µm). The slope of the polarization spectrum was investigated by defining the quantity R DC = p D /p C , where p C and p D represent polarization degrees in bands C and D, respectively. We find a clear correlation between R DC and the molecular hydrogen column density across the cloud. A positive slope (R DC > 1) dominates the lower density and well illuminated portions of the cloud, that are heated by the high mass star Oph S1, whereas a transition to a negative slope (R DC < 1) is observed toward the denser

show abstract

mentioning

confidence: 80%

The Far-infrared Polarization Spectrum of ρ Ophiuchi A from HAWC+/SOFIA Observations

Santos

Chuss

Dowell

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…We probed the plane-of-sky magnetic field, B sky , using the modified Davis-Chandrasekhar-Fermi method (DCF method) proposed by Cho & Yoo (2016). We have obtained magnetic strengths 17 times lower than previous estimates along the west rim (Soler et al 2018). The difference stems from (i) the selection of regions with little H i confusion along the lines of sight, (ii) refined estimates of the gas shell depths along the lines of sight, and (iii) the correction of the dispersion in polarisation angles due to the pile-up of independent eddies along the line of sight.…”

Section: Magnetic Field In the Superbubblementioning

confidence: 97%

Gas shells and magnetic fields in the Orion-Eridanus superbubble

Joubaud

Grenier

Ballet

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

Aims. The Orion-Eridanus superbubble has been blown by supernovae and supersonic winds of the massive stars in the Orion OB associations. It is the nearest site at which stellar feedback on the interstellar medium that surrounds young massive clusters can be studied. The formation history and current structure of the superbubble are still poorly understood, however. It has been pointed out that the picture of a single expanding object should be replaced by a combination of nested shells that are superimposed along the line of sight. We have investigated the composite structure of the Eridanus side of the superbubble in the light of a new decomposition of the atomic and molecular gas. Methods. We used H i 21 cm and CO (J=1−0) emission lines to separate coherent gas shells in space and velocity, and we studied their relation to the warm ionised gas probed in H α emission, the hot plasma emitting X-rays, and the magnetic fields traced by dust polarised emission. We also constrained the relative distances to the clouds using dust reddening maps and X-ray absorption. We applied the Davis-Chandrasekhar-Fermi method to the dust polarisation data to estimate the plane-of-sky components of the magnetic field in several clouds and along the outer rim of the superbubble. Results. Our gas decomposition has revealed several shells inside the superbubble that span distances from about 150 pc to 250 pc. One of these shells forms a nearly complete ring filled with hot plasma. Other shells likely correspond to the layers of swept-up gas that is compressed behind the expanding outer shock wave. We used the gas and magnetic field data downstream of the shock to derive the shock expansion velocity, which is close to ∼20 km s −1 . Taking the X-ray absorption by the gas into account, we find that the hot plasma inside the superbubble is over-pressured compared to plasma in the Local Bubble. The plasma comprises a mix of hotter and cooler gas along the lines of sight, with temperatures of (3-9) and (0.3 − 1.2) × 10 6 K, respectively. The magnetic field along the western and southern rims and in the approaching wall of the superbubble appears to be shaped and compressed by the ongoing expansion. We find plane-of-sky magnetic field strengths from 3 to 15 µG along the rim.

show abstract

“…However, it is clear that the density and B are not entirely isotropic in the vicinity of the Sun, and toward the nearby clouds we may be observing the N H and B ⊥ configuration in the walls of the cavity of hot ionized gas that extends all around the Sun, known as the Local Bubble (see Alves et al 2018, and references therein), the expanding supernova remnant known as the Orion-Eridanus superbubble (see Soler et al 2018, and references therein), and other nearby superbubbles (see, e.g., Bally 2008). These magnetized superbubbles would generate anisotropies in the mean direction of the magnetic field ( B ) that would favor the observations of B close to parallel to the plane of the sky.…”

Section: Projection Onto the Plane Of The Skymentioning

confidence: 99%

Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure

Soler

2019

A&A

Self Cite

View full text Add to dashboard Cite

We present a study of the relative orientation between the magnetic field projected onto the plane of sky (B ⊥ ) on scales down to 0.4 pc, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the distribution of gas column density (N H ) structures on scales down to 0.026 pc, derived from the observations by Herschel in submillimeter wavelengths, toward ten nearby (d < 450 pc) molecular clouds. Using the histogram of relative orientation technique in combination with tools from circular statistics, we found that the mean relative orientation between N H and B ⊥ toward these regions increases progressively from 0 • , where the N H structures lie mostly parallel to B ⊥ , with increasing N H , in many cases reaching 90 • , where the N H structures lie mostly perpendicular to B ⊥ . We also compared the relative orientation between N H and B ⊥ and the distribution of N H , which is characterized by the slope of the tail of the N H probability density functions (PDFs). We found that the slopes of the N H PDF tail are steepest in regions where N H and B ⊥ are close to perpendicular. This coupling between the N H distribution and the magnetic field suggests that the magnetic fields play a significant role in structuring the interstellar medium in and around molecular clouds. However, we found no evident correlation between the star formation rates, estimated from the counts of young stellar objects, and the relative orientation between N H and B ⊥ in these regions.

show abstract

The magnetic environment of the Orion-Eridanus superbubble as revealed by Planck

Cited by 38 publications

References 48 publications

The Far-infrared Polarization Spectrum of ρ Ophiuchi A from HAWC+/SOFIA Observations

The Far-infrared Polarization Spectrum of ρ Ophiuchi A from HAWC+/SOFIA Observations

Gas shells and magnetic fields in the Orion-Eridanus superbubble

Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure

Contact Info

Product

Resources

About