Detection of Hot Gas in the Interstellar Medium

Huang, Jiasheng; Songaila, A.; Cowie, L. L.; Jenkins, Edward B.

doi:10.1086/176128

Cited by 18 publications

(17 citation statements)

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“…Collisional ionization equilibrium (CIE) simulations of the LB powered by the missing stars of the subgroup B1 of Pleiades (BB02) within a turbulent interstellar medium (Breitschwerdt & de Avillez 2006, BA06;de Avillez & Breitschwerdt 2009, AB09) reproduced the clumpy distribution of Ovi, as well as its column density and dispersion inside the LB cavity observed by Copernicus (Jenkins 1978;Shelton & Cox 1994) and FUSE (Oegerle et al 2005;Savage & Lehner 2006), and the lack of Civ and Nv ions in the bubble, which is consistent with the observations with Copernicus (York 1977), IUE (Bruhweiler et al 1980), and GHRS-HST (Bertin et al 1995;Huang et al 1995). These observations point to column densities N(Civ) < 7 × 10 11 , N(Nv) < 3 × 10 12 cm −2 , log[N(Civ)/N(Ovi)] −0.9 and log[N(Nv)/N(Ovi)] −1.0.…”

Section: Introductionsupporting

confidence: 72%

Non-equilibrium ionization modeling of the Local Bubble

Avillez

Breitschwerdt

2012

A&A

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Aims. We present the first high-resolution non-equilibrium ionization simulation of the joint evolution of the Local Bubble (LB) and Loop I superbubbles in the turbulent supernova-driven interstellar medium (ISM). The time variation and spatial distribution of the Li-like ions Civ, Nv, and Ovi inside the LB are studied in detail.Methods. This work uses the parallel adaptive mesh refinement code EAF-PAMR coupled to the newly developed atomic and molecular plasma emission module E(A+M)PEC, featuring the time-dependent calculation of the ionization structure of H through Fe, using the latest revision of solar abundances. The finest AMR resolution is 1 pc within a grid that covers a representative patch of the Galactic disk (with an area of 1 kpc 2 in the midplane) and halo (extending up to 10 kpc above and below the midplane). Results. The evolution age of the LB is derived by the match between the simulated and observed absorption features of the Li-like ions Civ, Nv, and Ovi. The modeled LB current evolution time is bracketed between 0.5 and 0.8 Myr since the last supernova reheated the cavity in order to have N(Ovi) < 8 × 10 12 cm −2 , log[N(Civ)/N(Ovi)] < −0.9 and log[N(Nv)/N(Ovi)] < −1 inside the simulated LB cavity, as found in Copernicus, IUE, GHRS-IST and FUSE observations.

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Section: Introductionsupporting

confidence: 72%

Non-equilibrium ionization modeling of the Local Bubble

Avillez

Breitschwerdt

2012

A&A

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“…The presence of high-velocity (HV) absorption features of ionized gas between -120 km s −1 v LSR -80 km s −1 was detected in multiple lines of sight towards Orion (Cowie et al 1979;Welty et al 2002). In addition, intermediate-velocity (IV) features were detected between -80 km s −1 v LSR -20 km s −1 (Cowie & York 1978;Cowie et al 1979;Huang et al 1995;Welty et al 2002). Both components show similar depletions, ion ratios, and physical conditions, albeit the IV gas contains column densities that exceed that of the HV gas by a factor of 3 (e.g., Welty et al 2002).…”

Section: High-and Intermediate Velocity Gasmentioning

confidence: 98%

“…Figure 4 shows Hα velocity maps from the WHAM Hα spectral survey (Haffner et al 2003) of the Orion-Eridanus superbubble, covering the velocity space between -80 km s −1 v LSR +80 km s −1 . Overplotted are sightlines from absorption line studies (Cowie & York 1978;Cowie et al 1979;Huang et al 1995;Welty et al 2002). The HV and IV gas trace structures around Barnard's Loop and the λ Ori ring that extend outside of the traditional limits of the Orion-Eridanus superbubble (Reynolds & Ogden 1979;Heiles et al 1999;Bally 2008;Pon et al 2014a), as demonstrated by the sightlines of κ Ori, λ Ori, and λ Eri.…”

Section: High-and Intermediate Velocity Gasmentioning

confidence: 99%

“…We defer a thorough discussion of the Barnard's Loop bubble and its connection to the HV gas to section 4. (Cowie & York 1978;Cowie et al 1979;Huang et al 1995;Welty et al 2002) that show both high-velocity and intermediate-velocity gas (inverted triangles), lines of sight that show only intermediate-velocity gas (diamonds), and lines of sight that do not show a clear detection of high-velocity or intermediate-velocity gas (squares). The classes are plotted in different gray scalings to make them discernable, and we have explicitely labeled some of the stars in the lower right panel for orientation.…”

Section: Barnard's Loop Bubblementioning

confidence: 99%

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Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Ochsendorf

Brown

Bally

et al. 2015

ApJ

117

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The Orion-Eridanus superbubble is the prototypical superbubble due to its proximity and evolutionary state. Here, we provide a synthesis of recent observational data from WISE and Planck with archival data, allowing to draw a new and more complete picture on the history and evolution of the Orion-Eridanus region. We discuss the general morphological structures and observational characteristics of the superbubble, and derive quantitative properties of the gas-and dust inside Barnard's Loop. We reveal that Barnard's Loop is a complete bubble structure which, together with the λ Ori region and other smaller-scale bubbles, expands within the Orion-Eridanus superbubble. We argue that the Orion-Eridanus superbubble is larger and more complex than previously thought, and that it can be viewed as a series of nested shells, superimposed along the line of sight. During the lifetime of the superbubble, H II region champagne flows and thermal evaporation of embedded clouds continuously mass-load the superbubble interior, while winds or supernovae from the Orion OB association rejuvenate the superbubble by sweeping up the material from the interior cavities in an episodic fashion, possibly triggering the formation of new stars that form shells of their own. The steady supply of material into the superbubble cavity implies that dust processing from interior supernova remnants is more efficient than previously thought. The cycle of mass-loading, interior cleansing, and star formation repeats until the molecular reservoir is depleted or the clouds have been disrupted. While the nested shells come and go, the superbubble remains for tens of millions of years.

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“…The expansion speed of the superbubble was initially estimated to be 15 km s −1 (Menon 1957;Reynolds & Ogden 1979), but more recent estimates place the expansion velocity closer to 40 km s −1 (Cowie & York 1978;Cowie et al 1979;Brown et al 1995;Huang et al 1995;Welty et al 2002;Ochsendorf et al 2015).…”

Section: Tablementioning

confidence: 99%

Kompaneets Model Fitting of the Orion–eridanus Superbubble. Ii. thinking Outside of Barnard’s Loop

Pon

Ochsendorf

Bally³

et al. 2016

ApJ

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The Orion star-forming region is the nearest active high-mass star-forming region and has created a large superbubble, the Orion-Eridanus superbubble. Recent work by Ochsendorf et al. has extended the accepted boundary of the superbubble. We fit Kompaneets models of superbubbles expanding in exponential atmospheres to the new, larger shape of the Orion-Eridanus superbubble. We find that this larger morphology of the superbubble is consistent with the evolution of the superbubble being primarily controlled by expansion into the exponential Galactic disk ISM if the superbubble is oriented with the Eridanus side farther from the Sun than the Orion side. Unlike previous Kompaneets model fits that required abnormally small scale heights for the Galactic disk (<40 pc), we find morphologically consistent models with scale heights of 80 pc, similar to that expected for the Galactic disk.

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Detection of Hot Gas in the Interstellar Medium

Cited by 18 publications

References 0 publications

Non-equilibrium ionization modeling of the Local Bubble

Non-equilibrium ionization modeling of the Local Bubble

Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Kompaneets Model Fitting of the Orion–eridanus Superbubble. Ii. thinking Outside of Barnard’s Loop

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