by kovil » Sun Apr 09, 2006 4:18 am
Harry,
I was perusing the APJ back issues and found this one, here is a section,
from a paper about "Challenging Cosmic-Ray Propagation with Antiprotons: Evidence for a "Fresh" Nuclei Component?"
April 1, 2003 issue APJ { I inserted these ?'s or comments}
3. THE LB HYPOTHESIS
The low-density region around the Sun, filled with hot H I gas, is called the Local Bubble (see, e.g., Sfeir et al. 1999). The size of the region is about 200 pc {200 parsecs}, and it is likely that it was produced in a series of SN {supernova} explosions. Most probably its progenitor was an OB star association. Although people discuss different scenarios (see, e.g., Maíz-Apellániz 2001; Berghöfer & Breitschwerdt 2002), the Local Bubble (LB) age and the number of SN progenitors appear to be similar, 10 Myr {10 million years} and 1020 SNs, respectively. Most probably they exploded as core-collapse SNs II or thermonuclear SNs Ib/c with a mass of pre-SN stars between several and 10 M {10 solar masses}, with the last SN explosion occurring approximately 12 Myr ago, or three SNs occurring within the last 5 Myr.
There is also some evidence of an SN explosion nearby. An excess of 60Fe measured in a deep ocean core sample of ferromanganese crust suggests the deposition of SN-produced iron on Earth (Knie et al. 1999). The enhanced concentrations were found in two of three layers corresponding to a time span of less than 2.8 Myr and 3.7-5.9 Myr, respectively. The study suggests an SN explosion about 5 Myr ago at 30 pc distance. Another study reports an enhancement in the CR {cosmic ray} intensity dated about 40 kyr {40 thousand years ago} ago (Sonett, Morfill, & Jokipii 1987), which is interpreted as the passage across the solar system of the shock wave from an SN exploding about 0.1 Myr ago. Taking into account possible errors of all these estimates, they point to a nearby SN explosion some 1 Myr ago (see also discussion in Benítez, Maíz-Apellániz, & Canelles 2002).
{eta Carinae has had company recently ! , tho not as massive as eta is}
It could also be that fresh LB contributions from continuous acceleration in the form of shock waves (Bykov & Fleishman 1992) and/or energetic particles coming directly from SN remnants still influence the spectra and abundances of local CRs. The elemental abundances of the low-energy nonthermal component in a superbubble can differ strongly from the standard cosmic abundances (Bykov 2001) because of ejection of matter enriched with heavy elements from SNs and stellar winds of massive stars (Wolf-Rayet, OB stars). The continuous acceleration is connected with the lifetime of a shock wave in the LB. A reasonable estimate is given by the sound crossing time, approximately 2 Myr, for a distance of 200 pc in a 106 K plasma (Berghöfer & Breitschwerdt 2002). On the other hand, the particle crossing time can be estimated as t x2/D 1 Myr for a typical value of the diffusion coefficient in the ISM D 1028 cm s-2 and x 200 pc. Therefore, accelerated particles are expected to be present in this region.
========
SN Fe60 pennies from heaven keep falling on my head . . .
I had no idea the local bubble was so recently active, or that evidence for suggesting so had been discovered, I mean. With all the brown dwarf stars around nearby, and the abundance of heavy elements on earth, I figured we must be close to a local production area or the galactic winds have blown it to here, and I was wondering which was the case and was leaning in the local production direction, (as Ockam's Razor would say that is the simpler answer, as Qev? pointed out)
We are on the cusp of a new begining in data. APJ is currently in a shift over phase to using AASTeX v5.2 for submitted papers, and their online publishing is at an important gearing up moment. 268 astronomical data gathering sites are currently being linked up in a data base for referencing by paper writers for simplifying data retrieval by readers and researchers. What an age !!
Kovil
Harry,
I was perusing the APJ back issues and found this one, here is a section,
from a paper about "Challenging Cosmic-Ray Propagation with Antiprotons: Evidence for a "Fresh" Nuclei Component?"
April 1, 2003 issue APJ { I inserted these ?'s or comments}
3. THE LB HYPOTHESIS
The low-density region around the Sun, filled with hot H I gas, is called the Local Bubble (see, e.g., Sfeir et al. 1999). The size of the region is about 200 pc {200 parsecs}, and it is likely that it was produced in a series of SN {supernova} explosions. Most probably its progenitor was an OB star association. Although people discuss different scenarios (see, e.g., Maíz-Apellániz 2001; Berghöfer & Breitschwerdt 2002), the Local Bubble (LB) age and the number of SN progenitors appear to be similar, 10 Myr {10 million years} and 1020 SNs, respectively. Most probably they exploded as core-collapse SNs II or thermonuclear SNs Ib/c with a mass of pre-SN stars between several and 10 M {10 solar masses}, with the last SN explosion occurring approximately 12 Myr ago, or three SNs occurring within the last 5 Myr.
There is also some evidence of an SN explosion nearby. An excess of 60Fe measured in a deep ocean core sample of ferromanganese crust suggests the deposition of SN-produced iron on Earth (Knie et al. 1999). The enhanced concentrations were found in two of three layers corresponding to a time span of less than 2.8 Myr and 3.7-5.9 Myr, respectively. The study suggests an SN explosion about 5 Myr ago at 30 pc distance. Another study reports an enhancement in the CR {cosmic ray} intensity dated about 40 kyr {40 thousand years ago} ago (Sonett, Morfill, & Jokipii 1987), which is interpreted as the passage across the solar system of the shock wave from an SN exploding about 0.1 Myr ago. Taking into account possible errors of all these estimates, they point to a nearby SN explosion some 1 Myr ago (see also discussion in Benítez, Maíz-Apellániz, & Canelles 2002).
{eta Carinae has had company recently ! , tho not as massive as eta is}
It could also be that fresh LB contributions from continuous acceleration in the form of shock waves (Bykov & Fleishman 1992) and/or energetic particles coming directly from SN remnants still influence the spectra and abundances of local CRs. The elemental abundances of the low-energy nonthermal component in a superbubble can differ strongly from the standard cosmic abundances (Bykov 2001) because of ejection of matter enriched with heavy elements from SNs and stellar winds of massive stars (Wolf-Rayet, OB stars). The continuous acceleration is connected with the lifetime of a shock wave in the LB. A reasonable estimate is given by the sound crossing time, approximately 2 Myr, for a distance of 200 pc in a 106 K plasma (Berghöfer & Breitschwerdt 2002). On the other hand, the particle crossing time can be estimated as t x2/D 1 Myr for a typical value of the diffusion coefficient in the ISM D 1028 cm s-2 and x 200 pc. Therefore, accelerated particles are expected to be present in this region.
========
SN Fe60 pennies from heaven keep falling on my head . . .
I had no idea the local bubble was so recently active, or that evidence for suggesting so had been discovered, I mean. With all the brown dwarf stars around nearby, and the abundance of heavy elements on earth, I figured we must be close to a local production area or the galactic winds have blown it to here, and I was wondering which was the case and was leaning in the local production direction, (as Ockam's Razor would say that is the simpler answer, as Qev? pointed out)
We are on the cusp of a new begining in data. APJ is currently in a shift over phase to using AASTeX v5.2 for submitted papers, and their online publishing is at an important gearing up moment. 268 astronomical data gathering sites are currently being linked up in a data base for referencing by paper writers for simplifying data retrieval by readers and researchers. What an age !!
Kovil