3D3C Real Virtual Worlds Defined

Sivan, Yesha Y.

doi:10.4018/978-1-61692-808-7.ch002

Cited by 3 publications

(3 citation statements)

References 6 publications

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“…This emission is not part of a cataloged galactic nebula or H II region (Sharpless 1959;Maršálková 1974;Neckel & Vehrenberg 1985). It is also too faint to be seen in the Hα survey by Sivan (1974) and lies too far off the plane to be covered in the optical emission line survey of the Milky Way by Parker et al (1979). However, some of its brighter regions are faintly visible on both first and second digital Palomar Observatory Sky Survey (POSS) red images.…”

Section: Observationsmentioning

confidence: 91%

Discovery of an Apparent High Latitude Galactic Supernova Remnant

Fesen

Neustadt

Black

et al. 2015

ApJ

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Deep Hα images of a faint emission complex 4.0 • × 5.5 • in angular extent and located far off the Galactic plane at l = 70.0 • , b = −21.5 • reveal numerous thin filaments suggestive of a supernova remnant's shock emission. Low dispersion optical spectra covering the wavelength range 4500 -7500 A show only Balmer line emissions for one filament while three others show a Balmer dominated spectrum along with weak [N I] 5198, 5200Å, [O I] 6300, 6364Å, [N II] 6583Å, [S II] 6716, 6731Å and in one case [O III] 5007Å line emission. Many of the brighter Hα filaments are visible in near UV GALEX images presumably due to C III] 1909Å line emission. ROSAT All Sky Survey images of this region show a faint crescent shaped X-ray emission nebula coincident with the portion of the Hα nebulosity closest to the Galactic plane.The presence of long, thin Balmer dominated emission filaments with associated UV emission and coincident X-ray emission suggests this nebula is a high latitude Galactic supernova remnant despite a lack of known associated nonthermal radio emission. Relative line intensities of the optical lines in some filaments differ from commonly observed [S II]/Hα ≥ 0.4 radiative shocked filaments and typical Balmer filaments in supernova remnants. We discuss possible causes for the unusual optical SNR spectra. Subject headings: ISM: individual objects: G70.0-21.5, ISM: supernova remnant -shock waves -optical -X-rays: ISM

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Section: Observationsmentioning

confidence: 91%

Discovery of an Apparent High Latitude Galactic Supernova Remnant

Fesen

Neustadt

Black

et al. 2015

ApJ

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“…45 • elongated superbubble structure, with enhanced Hα flux within the confines of the bubble (e.g. Pickering 1890; Barnard 1894;Elliott & Meaburn 1970;Elliott 1973;Isobe 1973;Reynolds, Roesler & Scherb 1974;Sivan 1974;Johnson 1978;Reynolds & Ogden 1979;Boumis et al 2001;Haffner et al 2003). The east side of the superbubble is dominated by a bright crescent of Hα emission, which is referred to as Barnard's Loop (Pickering 1890;Barnard 1894).…”

Section: Orion-eridanus Superbubblementioning

confidence: 99%

Kompaneets model fitting of the Orion–Eridanus superbubble

Pon¹,

Johnstone²,

Bally³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Winds and supernovae from OB associations create large cavities in the interstellar medium referred to as superbubbles. The Orion molecular clouds are the nearest highmass star-forming region and have created a highly elongated, 20 • x 45 • , superbubble. We fit Kompaneets models to the Orion-Eridanus superbubble and find that a model where the Eridanus side of the superbubble is oriented away from the Sun provides a marginal fit. Because this model requires an unusually small scaleheight of 40 pc and has the superbubble inclined 35 • from the normal to the Galactic plane, we propose that this model should be treated as a general framework for modelling the Orion-Eridanus superbubble, with a secondary physical mechanism not included in the Kompaneets model required to fully account for the orientation and elongation of the superbubble.

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“…As the Ori OB1 association evolved, the ionization photons and stellar winds from massive stars and supernova ejectra produced the Orion-Eridanus Superbubble (Brown et al 1995). The Orion-Eridanus Superbubble has been studied in many wavelengths (reviews by Heiles et al 1999), e.g., in H I (Heiles 1976;Brown et al 1995), IRAS 100 µm (Burrows et al 1993), Hα (Sivan 1974;Reynolds & Ogden 1979), X rays (Burrows et al 1993;Snowden et al 1995;Guo et al 1995), and γ rays (Parizot 1998).…”

Section: Introductionmentioning

confidence: 99%

Triggered Star Formation on the Border of the Orion-Eridanus Superbubble

Lee

Chen

2009

ApJ

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A census of classical T Tauri stars and Herbig Ae/Be stars has been performed around the Orion-Eridanus Superbubble which is ionized and created by the Ori OB1 association. This sample is used to study the spatial distribution of newborn stars, hence the recent star formation sequence, in the region that includes two giant molecular clouds (Orion A and B) and additional smaller clouds (NGC 2149, GN 05.51.4, VdB 64, the Crossbones, the Northern Filament, LDN 1551, LDN 1558, and LDN 1563. Most of the molecular clouds are located on the border of the Superbubble, and associated with Hα filaments and star formation activity, except the Northern Filament which is probably located outside the Superbubble. This suggests that while star formation progresses from the oldest Ori OB1a subgroup to 1b, 1c and 1d, the Superbubble compresses and initiates starbirth in clouds such as NGC 2149, GN 05.51.4, VdB 64, and the Crossbones, which are located more than one hundred pc away from the center of the Superbubble, and even in clouds some two hundred pc away, i.e., in LDN 1551, LDN 1558, and LDN 1563. A superbubble appears to have potentially a long-range influence in triggering next-generation star formation in an OB association.

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3D3C Real Virtual Worlds Defined

Cited by 3 publications

References 6 publications

Discovery of an Apparent High Latitude Galactic Supernova Remnant

Discovery of an Apparent High Latitude Galactic Supernova Remnant

Kompaneets model fitting of the Orion–Eridanus superbubble

Triggered Star Formation on the Border of the Orion-Eridanus Superbubble

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