The UvA-LINKER will give you a range of other options to find the full text of a publication (including a direct link to the full-text if it is located on another database on the internet).
De UvA-LINKER biedt mogelijkheden om een publicatie elders te vinden (inclusief een directe link naar de publicatie online als deze beschikbaar is in een database op het internet).

Search results

Query: journal id: "astrophysicalxjournal"

AuthorsS. van Straaten, M. van der Klis, R. Wijnands
TitleRelations Between Timing Features and Colors in Accreting Millisecond Pulsars
JournalAstrophysical Journal
Issuenr.1 part 1
FacultyFaculty of Science
Institute/dept.FNWI: Astronomical Institute Anton Pannekoek (IAP)
Keywordsaccretion disks; pulsars; X-ray stars
Classification39.22 astrofysica
AbstractWe have studied the aperiodic X-ray timing and color behavior of the accreting millisecond pulsars SAX J1808.4-3658, XTE J1751-305, XTE J0929-314, and XTE J1814-338 using large data sets obtained with the Rossi X-Ray Timing Explorer. We find that the accreting millisecond pulsars have timing properties very similar to atoll sources and low-luminosity bursters. On the basis of the correlation of timing and color behavior, SAX J1808.4-3658 can be classified as an atoll source, and XTE J0929-314 and XTE J1814-338 are consistent with atoll sources, but the color behavior of XTE J1751-305 is different. Unlike the color in other atoll sources, the hard color in the extreme island state of XTE J1751-305 is strongly correlated with soft color and intensity and is not anticorrelated with any of the characteristic frequencies. We found previously that the frequencies of the variability components of atoll sources follow a universal scheme of correlations. The frequency correlations of the accreting millisecond pulsars are similar, but in the cases of SAX J1808.4-3658 and XTE J0929-314 they are shifted compared with those of the other atoll sources in a way that is most easily described as a shift in upper and lower kilohertz quasi-periodic oscillation (QPO) frequency by a factor close to 1.5. However, we note that the shift in the lower kilohertz QPO frequency is based on only one observation for SAX J1808.4-3658. XTE J1751-305 and XTE J1814-338, as well as the low-luminosity bursters, show no or possibly only small shifts.
Note(c)1995 American Astronomical Society
Document typeArticle
Document finderUvA-Linker