Knee MRI. Part I: basic overview

Grenier, Julie-Marthe

doi:10.1016/s1479-2354(04)00019-7

Cited by 5 publications

(11 citation statements)

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“…The temporally resolved ccSN rate for the next 10 Myr within 600 pc yields 17.0 +4.5 −3.6 ccSNe/Myr and is shown in 14. Our result can be compared to the range from 20 to 27 ccSNe per Myr for the Gould Belt from Grenier (2004) and also with 21 ± 5 ccSNe/Myr from Hohle et al (2010). The value between 2 and 3 Myr, seen as a peak in Hohle et al (2010), is now consistent with a constant rate.…”

Section: Discussion On Supernova Progenitor Distributionsupporting

confidence: 71%

“…The observed volume is then calculated within the disc using the distances given in Table 8. Comparing the ccSN rate in the solar vicinity with the Galactic ccSN rate of 2.5 SNe per century (Tammann et al 1994) suggests that the current ccSN rate within 600 pc and 1 kpc is increased due to the Gould Belt as found by Grenier (2004) and Popov et al (2005) by about a factor of 5-6.…”

Section: Discussion On Supernova Progenitor Distributionmentioning

confidence: 76%

“…. 27 ccSNe/Myr for the Gould Belt from Grenier (2004) and to ≈ 20 ccSNe/Myr from Hohle et al (2010).…”

Section: B Calculations and Results Without Transformed Parallaxmentioning

confidence: 92%

“…The amount of 26 Al (Diehl et al 2006) implies a rate of (1.9±1.1) ccSNe per century in our Galaxy. Grenier (2004) found 20 to 27 SNe per Myr for the Gould Belt (Gould 1879), a local star forming region within 600 pc (for an historical overview, see Stothers & Frogel 1974), by studying observed star counts. This local current rate is 5 to 6 times higher than the Galactic average.…”

Section: Introductionmentioning

confidence: 99%

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Determination of a temporally and spatially resolved supernova rate from OB stars within 5 kpc

2014

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We spatially and temporally resolve the future Supernova (SN) rate in the Solar vicinity and the whole Galaxy by comparing observational parameters of massive stars with theoretical models for estimating age and mass and, hence, the remaining lifetime until the SN explosion. Our SN rate derived in time and space for the future (few Myr) should be the same as in the last few Myr by assuming a constant rate. From BVRIJHK photometry, parallax, spectral type, and luminosity class we compile a Hertzsprung-Russell diagram (HRD) for 25 027 massive stars and derive extinction, and luminosity, then mass, age, and remaining lifetime from evolutionary models. Within 600 pc our sample of SN progenitors and, hence, SN prediction, is complete, and all future SN events of our sample stars take place in 8 % of the area of the sky, whereas 90 % of the events take place in 7 % of the area of the sky. The current SN rate within 600 pc is increased by a factor of 5-6 compared with the Galactic rate. For a distance of 5 kpc our sample is incomplete, nevertheless 90 % of those SN events take place in only 12 % of the area of the projected sky. If the SN rate in the near future is the same as the recent past, there should be unknown young neutron stars concentrated in those areas. Our distribution can be used as input for constraints of gravitational waves detection and for neutron star searches.

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Section: Discussion On Supernova Progenitor Distributionsupporting

confidence: 71%

Section: Discussion On Supernova Progenitor Distributionmentioning

confidence: 76%

“…. 27 ccSNe/Myr for the Gould Belt from Grenier (2004) and to ≈ 20 ccSNe/Myr from Hohle et al (2010).…”

Section: B Calculations and Results Without Transformed Parallaxmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

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Determination of a temporally and spatially resolved supernova rate from OB stars within 5 kpc

2014

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“…the Gould Belt) and of the local birth rate. For example, the age of the Gould Belt is believed to be ∼10 7−8 yr (Grenier 2004). Because the birth rate of the canonical pulsars in the Gould Belt is expected to be one per 10 5 yr, and because the birth rates of the MSPs in the Galactic field are 2-3 orders smaller than that of the canonical pulsars, one may expect 1 per 10 7−8 yr as the birth rate of the MSPs in the Gould Belt.…”

Section: Galactic Distribution Of Mspsmentioning

confidence: 99%

Population study for γ-ray pulsars with the outer gap model - II. Millisecond pulsars

Takata¹,

Wang²,

Cheng³

2011

Monthly Notices of the Royal Astronomical Society

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The population of γ‐ray emitting millisecond pulsars (MSPs) was studied by using Monte Carlo techniques. We simulated the Galactic distributions of the MSPs, and applied the outer gap model for the γ‐ray emission from each simulated MSP. We took into account the dependence of the observed γ‐ray flux on the viewing angle and on the inclination angle, which is the angle between the rotation axis and the magnetic axis, respectively. Using the sensitivity of the 6‐month long observation of the Fermi telescope and radio sensitivities of existing pulsar surveys, 9–13 radio‐selected and 22–35 γ‐ray‐selected pulsars are detected within our simulation. The statistical properties of the simulated population are consistent with the Fermi observations. Scaling the observed sensitivity , where T is the length of observation time, the present model predicts that over the 5‐year mission Fermi would detect 15–22 radio‐selected γ‐ray MSPs, and 95–152 γ‐ray‐selected MSPs. Our simulation also predicts that about 100 (or 200–300) γ‐ray MSPs with a flux larger than F≥ 10−11 erg cm−2 s−1 (or 5 × 10−12 erg cm−2 s−1) irradiate the Earth. With the present sensitivities of radio surveys, most of them are categorized as γ‐ray‐selected pulsars, indicating that most of the γ‐ray MSPs have been missed by the present Fermi observations. We argue that the Galactic Fermi unidentified sources located at high latitudes should be dominated by MSPs, whereas the sources in the Galactic plane are dominated by radio‐quiet canonical pulsars. We want to emphasize that the predicted number of radio‐loud γ‐ray MSPs depends on the sensitivities of radio surveys and that it can be increased, for example, from 15–22 to 26–37 if the radio sensitivity is improved by a factor of 2.

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OB Stars in the Solar Neighborhood. I. Analysis of their Spatial Distribution

Elías¹,

Cabrera-Caño²,

Alfaro³

2006

Astron J

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We present a newly-developed, three-dimensional spatial classification method, designed to analyze the spatial distribution of early type stars within the 1 kpc sphere around the Sun. We propose a distribution model formed by two intersecting disks -the Gould Belt (GB) and the Local Galactic Disk (LGD)defined by their fundamental geometric parameters. Then, using a sample of about 550 stars of spectral types earlier than B6 and luminosity classes between III and V, with precise photometric distances of less than 1 kpc, we estimate for some spectral groups the parameters of our model, as well as single membership probabilities of GB and LGD stars, thus drawing a picture of the spatial distribution of young stars in the vicinity of the Sun.

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Knee MRI. Part I: basic overview

Cited by 5 publications

References 0 publications

Determination of a temporally and spatially resolved supernova rate from OB stars within 5 kpc

Determination of a temporally and spatially resolved supernova rate from OB stars within 5 kpc

Population study for γ-ray pulsars with the outer gap model - II. Millisecond pulsars

OB Stars in the Solar Neighborhood. I. Analysis of their Spatial Distribution

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