The EUV source population and the local bubble

Warwick, R. S.; Barber, C. R.; Hodgkin, S. T.; Pye, J. P.

doi:10.1093/mnras/262.2.289

Cited by 42 publications

(27 citation statements)

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“…The Local Hot Bubble (LHB), also called the Local Bubble, is a large (diameter D50È100 pc), di †use (n D 0.05 cm~3), presumably hot K), X-ray emissive region (T c \ 106 containing the Sun (Snowden et al 1990 ;Warwick et al 1993 ;Cox & Reynolds 1987). The LHB is situated within a cavity called the Local Cavity.…”

Section: Application To the L Ocal Hot Bubblementioning

confidence: 99%

Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X‐Ray Emission

Shelton¹

1999

ApJ

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This paper provides detailed descriptions of the X-ray emission from supernova remnants (SNRs) evolving in warm, low-density, nonthermal pressureÈdominated regions K, n \ 0.001 cm~3, (T 0 \ 104 or 7200 K cm~3). Nonequilibrium ionization hydrocode simulations are used to predict the P nt \ 1800 high-resolution spectra, and keV ROSAT PSPC count rates, spatial appearance, color temperatures, 1 4 3 4 and ratios of O VII to O VIII emission-line Ñuxes as a function of time. If undisturbed, the remnants are quite long lived, surviving for D1.2 ] 107 to D1.6 ] 107 yr. During their brief energy-conserving phases, the hot, highly pressurized gas behind their shock fronts copiously emits X-rays. Thus, their keV 1 4 surface brightnesses are thousands of ROSAT PSPC counts s~1 arcmin~2 and the remnants appear strongly edge brightened. The onset of the radiative phase heralds the end of the extreme X-ray luminosities but not the end of the X-ray emission. After the cool shell forms behind the shock front, the hot SNR bubble slowly radiates away the remaining energy, with a diminutive fraction released in the form of X-rays. Thus, the keV surface brightnesses are tens to hundreds of ROSAT PSPC counts s~1 1 4 arcmin~2 and the remnants appear "" centrally Ðlled.ÏÏ The hot plasma within the remnant bubbles is always out of collisional ionizational equilibrium. Early on, the ionization states are much lower than expected for such hot gas. Later on, the ionization states are higher. This paper also applies the standard observational analyses for determining the color temperature, electron density, and thermal pressure to ROSAT "" observations ÏÏ of one of the simulated remnants, thus providing a map between observational results and physical conditions. The paper reports the O`5, N`4, and C`3 column densities for the simulated remnants. The simulations may be of interest and are applied to studies of the Galactic halo and Local Bubble. They may also be of interest to studies of external galaxies and interarm regions of the Milky Way.

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Section: Application To the L Ocal Hot Bubblementioning

confidence: 99%

Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X‐Ray Emission

Shelton¹

1999

ApJ

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“…The fraction of this cavity filled with extremely hot gas (T ≈ 10 6 K) is known as the Local Hot Bubble (LHB) (e.g., Paresce 1984;Cox & Reynolds 1987;Snowden et al 1990;Warwick et al 1993;Leroy 1999;Sfeir et al 1999;Breitschwerdt et al 2000;Lallement et al 2003;Welsh & Lallement 2005).…”

Section: Introductionmentioning

confidence: 99%

Mapping the interface between the Local and Loop I bubbles using Strömgren photometry

Reis

Corradi²

2008

A&A

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Context. The Sun is located inside an extremely low density region of quite irregular shape called the Local Bubble or Local Cavity. The fraction of this cavity filled with extremely hot gas is known as the Local Hot Bubble. Close to the Local Bubble, there is an even larger cavity known as Loop I. A ring-like feature observed in X-ray and Hi has been proposed as the contour of the bubbles interaction zone around 70 pc. Aims. Our goal is to identify the interface between the Local and Loop I Bubbles and discuss the ring's existence using Strömgren uvbyHβ data. Methods. We have used the uvbyHβ data of the General Catalogue of Photometric Data, covering the region defined by the Galactic coordinates: 250• to obtain E(b − y) colour excess and distances. A set of exclusion criteria have been applied to eliminate the values inappropriate to the study of the interstellar reddening distribution. The final sample is composed of 4346 stars located up to 500 pc from the Sun. Conclusions. If the ring really exists the colour excess distribution indicates that it is very fragmented and distorted. However, the different characteristics of the reddening inside and along the ring do not support the existence of a ring.

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“…Based on a detailed analysis of the statistics pertaining to the ROSAT WFC survey, Warwick et al (1993) concluded that the effective edge of the local bubble in this region is anomalously close to the Sun i.e. at ~ 10 pc as opposed to a more typical radius for the bubble of 80-100 pc).…”

Section: Discussionmentioning

confidence: 99%

“…One feature of the local cool gas distribution which has been highlighted by the recent EUV all-sky surveys carried out by the ROSAT WFC and EUVE (Pounds et al 1993;Pye et al 1995;Bowyer et al 1994 ;Barber et al (1996) ) is an apparent nearby "wall" of absorption observed in the general direction of the Galactic centre as revealed by the relative paucity of EUV source detections in this region (e.g. Warwick et al 1993). Here we use a combination of EUV and X-ray data derived from the ROSAT all-sky survey to investigate the distribution of absorbing gas in the direction of this wall.…”

Section: Introductionmentioning

confidence: 96%

Mapping Cool Gas in the ISM with ROSAT

Hutchinson

Warwick

Willingale

1997

International Astronomical Union Colloquium

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Abstract. We have investigated the distribution of cool gas within the local interstellar medium (<150 pc) using data derived from both the ROSAT X-ray and EUV all-sky surveys. The EUV/X-ray spectra for a sample of 89 white dwarf stars and 200 active late-type stars have been analysed to give an estimate of the gas column density along each object's line of sight. In order to extend the sky coverage we have also included in the analysis 190 late-type stars detected only in the X-ray band. The derived NHI measurements confirm the size of the local low density bubble as typically 50-100 pc and also show that in the general direction of Loop I there is a substantial excess of absorption at a range of distances from 10-150 pc.

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The EUV source population and the local bubble

Cited by 42 publications

References 0 publications

Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X‐Ray Emission

Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X‐Ray Emission

Mapping the interface between the Local and Loop I bubbles using Strömgren photometry

Mapping Cool Gas in the ISM with ROSAT

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