A VLA Study of the Expansion of Tycho's Supernova Remnant

Reynoso, E. M.; Moffett, D. A.; Goss, W. M.; Dubner, G.; Dickel, John R.; Reynolds, Stephen P.; Giacani, E.

doi:10.1086/304997

Cited by 126 publications

(181 citation statements)

References 28 publications

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“…The data points in the figure give the temperatures determined along the rim from our fits, assuming that the X-ray emission is thermal (Table 4); the appropriate azimuthal angle is determined with reference to the center adopted by Reynoso et al (1997). The electron temperatures we measure are clearly much lower than the mean temperatures expected for shock velocities determined from the radio expansion, with electron-to-mean temperature ratios of 0.10-0.20.…”

Section: Electron Temperaturesmentioning

confidence: 79%

“…The faster expansion observed at the outer boundary corresponds to an average forward shock velocity of 4600 AE 400 (D=2:3 kpc) km s À1 , where D is the distance in kiloparsecs. The expansion of the radio boundary is also observed to vary with azimuthal angle (Strom, Goss, & Shaver 1982;Reynoso et al 1997). Strong deceleration in the east is caused by the remnant's interaction with dense H gas (Reynoso et al 1999).…”

Section: Introductionmentioning

confidence: 93%

“…The implied ratio of electron and mean particle temperatures is about 0.1, giving an electron-to-proton temperature ratio of about 0.07 (with l ¼ 7 for the N-enriched circumstellar material surrounding SN 1987A). The X-ray line profiles (observed with the high spectral resolution High-Energy Transmission Gratings on Reynoso et al (1997) vs. azimuthal angle, increasing counterclockwise from north. The scatter in the south and southwest (angles greater than 200 ) is attributed to uncertainties in the radio expansion from uncertainties in obtaining the radius.…”

Section: Electron Temperaturesmentioning

confidence: 99%

“…Strong deceleration in the east is caused by the remnant's interaction with dense H gas (Reynoso et al 1999). Although the outer boundaries of the X-ray and radio emission show excellent correspondence, the average expansions measured at these wavelengths are inconsistent: the expansion rate m, defined so that the time evolution of the remnant radius is r $ t m , is 0:471 AE 0:028 in the radio (Reynoso et al 1997) and 0:71 AE 0:06 for the outer radii in X-rays (Hughes 2000). This discrepancy is unresolved, but appears to be a common pattern in young remnants, such as Cas A (Koralesky et al 1998;Vink et al 1998) and Kepler's SNR (Dickel et al 1988;Hughes 1999).…”

Section: Introductionmentioning

confidence: 99%

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Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

Hwang

Decourchelle

Holt

et al. 2002

ApJ

161

172

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We present Chandra X-ray images of Tycho's supernova remnant that delineate its outer shock as a thin, smooth rim along the straight northeastern edge and most of the circular western half. The images also show that the Si and S ejecta are highly clumpy and have reached near the forward shock at numerous locations. Most of the X-ray spectra that we examine along the rim show evidence of line emission from Si and S ejecta, while the continuum is well represented by either a thermal or a nonthermal model. If the continuum is assumed to be thermal, the electron temperatures at the rim are all similar at about 2 keV, while the ionization ages are very low because of the overall weakness of the line emission. These electron temperatures are substantially below those expected for equilibration of the electron and ion temperatures, assuming shock velocities inferred from radio and X-ray expansion measurements; the electron-to-mean temperature ratios are d0.1-0.2, indicating that collisionless heating of the electrons at the shock is modest. The nonthermal contribution to these spectra might be important, but cannot be strongly constrained by these data. It could account for as much as half of the flux in the 4-6 keV energy range, based on an extrapolation of the hard X-ray spectrum above 10 keV.

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Section: Electron Temperaturesmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 93%

Section: Electron Temperaturesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

Hwang

Decourchelle

Holt

et al. 2002

ApJ

161

172

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“…The size of the remnant on the sky is 8 × 5 , which corresponds to 5.3 pc×3.3 pc at the distance of the remnant, known to be of 2.3 kpc (Chevalier et al 1980). The remnant has been extensively studied in X-rays (Hwang et al 1998;Hwang & Gotthelf 1997;Vancura et al 1995;Fink et al 1994), radio (Velázquez et al 1998;Reynoso et al 1997), and optical (Smith et al 1991). The IR studies of Tycho are very scarce.…”

Section: Tychomentioning

confidence: 99%

Dust in the Tycho, Kepler and Crab supernova remnants

Douvion

Lagage

Césarsky

et al. 2001

A&A

118

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Abstract. SuperNova Remnants (SNR) have been extensively studied in radio, X-rays and optical, but barely in the InfraRed (IR). From IRAS observations, SNR are known to be IR emitters, but the origin of the emission is difficult to assess because of the limited angular and spectral resolution of IRAS observations. ISO follow-up observations of the Cassiopeia-A SNR have shown that the mid-IR radiation from this remnant was dominated by thermal emission from silicate condensates made from SN material. These condensates constitute a probe which can provide unique information about element mixing inside a SN. In this paper, we present ISOCAM observations of the three other young SNR's known in our galaxy: the Kepler SNR, the Tycho SNR and the Crab Nebula. The emission observed from the Kepler SNR is dominated by dust thermal emission. The dust at the origin of the IR emission is circumstellar, not from SN condensates. "Astronomical" silicates, collisionally heated to a temperature of 107 K, can account for both the mid-IR ISO data and the IRAS data. The IR emission from Tycho is probably also emitted by circumstellar or interstellar dust. In order to reproduce both the mid-IR ISO data and the IRAS data, a model with two dust components, one at a temperature of 107 K and the other at 55 K, is needed. The mid-IR emission from the Crab is dominated by synchrotron radiation; no dust is detected.

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Astrometry of the 1572 supernova (B Cassiopeiae)

Green

2004

Astron Nachr

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Abstract. Contemporary European measurements of the Milky Way supernova of 1572 (B Cas) have been analyzed to compute a modern position for the star in 1572. This work adds to that done by previous 20th-century authors by using a new procedure and previously unused astrometry by 16th-century European observers. Comparison is made with earlier analyses and to modern positional data on the supernova remnant (3C 10).

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A VLA Study of the Expansion of Tycho's Supernova Remnant

Cited by 126 publications

References 28 publications

Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

Dust in the Tycho, Kepler and Crab supernova remnants

Astrometry of the 1572 supernova (B Cassiopeiae)

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