Kompaneets model fitting of the Orion–Eridanus superbubble

Pon, Andy; Johnstone, Doug; Bally, John; Heiles, Carl

doi:10.1093/mnras/stu1704

Cited by 13 publications

(40 citation statements)

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“…Even though the definite extent of the IV gas should be established through an absorption line study that include sightlines covering the entire region shown in Fig. 4, here we argue that that the IV gas traces a structure significantly larger than the dimensions of the Orion-Eridanus superbubble described in previous works (Reynolds & Ogden 1979;Heiles et al 1999;Bally 2008;Pon et al 2014a).…”

Section: Discussioncontrasting

confidence: 51%

“…Nonetheless, it is possible that individual small-scale structures may still be too bright given their size and distance from Orion OB1 (Pon et al 2014b). Note that some of these filaments lie outside of what has previously been thought to be the edges of the Orion-Eridanus superbubble (Reynolds & Ogden 1979;Heiles et al 1999;Bally 2008;Pon et al 2014a). The dust temperatures measured inside the superbubble aperture and Barnard's Loop are similar to that observed for the entire diffuse sky by Planck (see discussion in Sec.…”

Section: Global Observational Characteristicsmentioning

confidence: 95%

“…In any case, the shock velocity of the IV gas (∼ 40 km s −1 ) is not fast enough to ionize hydrogen: therefore, the Eridanus filaments (and the IV gas) are photo-ionized by Orion OB1, which was already noted by Reynolds & Ogden (1979) and Welty et al (2002). We note that Pon et al (2014a) explored other mechanisms of ionization, but concluded that Orion OB1 most likely causes the observed ionization state of the IV gas. When the spherical geometry from Fig.…”

Section: Summary: the Structure Of The Orion-eridanus Superbubblementioning

confidence: 97%

“…The Orion-Eridanus superbubble is a nearby (∼400 pc) expanding structure that is thought to span 20 • × 45 • on the sky (Reynolds & Ogden 1979;Bally 2008;Pon et al 2014a). Because of its proximity and evolutionary stage, it is traced at a multitude of wavelengths (Heiles et al 1999), serving as a benchmark to the study of superbubbles.…”

Section: Introductionmentioning

confidence: 99%

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Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Ochsendorf

Brown

Bally

et al. 2015

ApJ

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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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Section: Discussioncontrasting

confidence: 51%

Section: Global Observational Characteristicsmentioning

confidence: 95%

Section: Summary: the Structure Of The Orion-eridanus Superbubblementioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Ochsendorf

Brown

Bally

et al. 2015

ApJ

Self Cite

117

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“…In semi-analytical calculations, the thin-shell approximation can be the key to obtaining the expansion of the super-bubble; for example, [5] [6] [7] [8] [9]. The Kompaneyets approximation, see [10] [11], has been used in order to model the super-bubble W4 [9] and the Orion-Eridanus super-bubble [12] [13]. The hydro-dynamical approximation, with the inclusion of interstellar density gradients, can produce a blowout into the galactic halo, see [14] [15].…”

Section: Introductionmentioning

confidence: 99%

Energy Conservation in the Thin Layer Approximation: VI. Bubbles and Super-Bubbles

Zaninetti¹

2021

IJAA

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We model the conservation of energy in the framework of the thin layer approximation for two types of interstellar medium (ISM). In particular, we analyse an ISM in the presence of self-gravity and a Gaussian ISM which produces an asymmetry in the advancing shell. The astrophysical targets to be simulated are the Fermi bubbles, the local bubble, and the W4 super-bubble. The theory of images is applied to a piriform curve, which allows deriving some analytical formulae for the observed intensity in the case of an optically thin medium.

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Cosmography of OB stars in the solar neighbourhood

Bouy

Alves

2015

A&A

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We construct a 3D map of the spatial density of OB stars within 500 pc from the Sun using the Hipparcos catalogue and find three large-scale stream-like structures that allow a new view on the solar neighbourhood. The spatial coherence of these blue streams and the monotonic age sequence over hundreds of parsecs suggest that they are made of young stars, similar to the young streams that are conspicuous in nearby spiral galaxies. The three streams are 1) the Scorpius to Canis Majoris stream, covering 350 pc and 65 Myr of star formation history; 2) the Vela stream, encompassing at least 150 pc and 25 Myr of star formation history; and 3) the Orion stream, including not only the well-known Orion OB1abcd associations, but also a large previously unreported foreground stellar group lying only 200 pc from the Sun. The map also reveals a remarkable and previously unknown nearby OB association, between the Orion stream and the Taurus molecular clouds, which might be responsible for the observed structure and star formation activity in this cloud complex. This new association also appears to be the birthplace of Betelgeuse, as indicated by the proximity and velocity of the red giant. If this is confirmed, it would solve the long-standing puzzle of the origin of Betelgeuse. The well-known nearby star-forming low-mass clouds, including the nearby T and R associations Lupus, Cha, Oph, CrA, Taurus, Vela R1, and various low-mass cometary clouds in Vela and Orion, appear in this new view of the local neighbourhood to be secondary star formation episodes that most likely were triggered by the feedback from the massive stars in the streams. We also recover well-known star clusters of various ages that are currently cruising through the solar neighbourhood. Finally, we find no evidence of an elliptical structure such as the Gould belt, a structure we suggest is a 2D projection effect, and not a physical ring.

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Kompaneets model fitting of the Orion–Eridanus superbubble

Cited by 13 publications

References 100 publications

Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Nested Shells Reveal the Rejuvenation of the Orion–eridanus Superbubble

Energy Conservation in the Thin Layer Approximation: VI. Bubbles and Super-Bubbles

Cosmography of OB stars in the solar neighbourhood

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