Sediment core chemistry data summary from the MQR Mound, August and December 1991 / submitted to Regulatory Division, New England Division, U.S. Army Corps of Engineers ; prepared by Peggy M. Murray ; submitted by Science Applications International Corportation.

Abstract

Grain Size Results 3.3 Chemistry Results 3.3.1 Pesticide/PCB Results 3.3.2 Metal Results 3.3.3 PAH Results 3.3.4 Volatile Organic Results 4.0 DISCUSSION 4. 1 Volume Estimates of MQR Source Materials 4.2 Metal Ratios of MQR Source Materials 4.3 Organic Contamination of MQR Sediments

Formation and evolution of compact binaries in globular clusters – II. Binaries with neutron stars

“…What is the CE efficiency, and is the NS spun up by accreting the material? What is the result of mass accretion on to a NS after it has experienced a merger, either in a binary due to unstable MT, or during a collision? What is the final fate of a mass‐transferring NS–WD binary? How does the evolution of a mass‐transferring NS–MS binary proceed when the companion's mass reaches ≲0.04 M ⊙ ? What is the dependence of qLMXB numbers on the cluster metallicity? This holds the potential to determine the cause of the LMXB metallicity dependence (see ).In particular, if future observations show that the metallicity dependence of qLMXBs follows that for bright LMXBs, it will most likely indicate that these two types of clusters had different IMFs (and thus star formation histories), as predicted by Grindlay (1993) and expected from star formation theory in dense metal‐rich environments (Murray 2007). If metal‐poor GCs have similar numbers of MSPs as metal‐rich GCs, but fewer qLMXBs (indicating a shorter LMXB lifetime), then the idea of irradiation‐induced winds is likely to be correct (Maccarone et al 2004).…”

“…In particular, if future observations show that the metallicity dependence of qLMXBs follows that for bright LMXBs, it will most likely indicate that these two types of clusters had different IMFs (and thus star formation histories), as predicted by Grindlay (1993) and expected from star formation theory in dense metal‐rich environments (Murray 2007). If metal‐poor GCs have similar numbers of MSPs as metal‐rich GCs, but fewer qLMXBs (indicating a shorter LMXB lifetime), then the idea of irradiation‐induced winds is likely to be correct (Maccarone et al 2004).…”