The Vitamins (A, B, and C) of Papaya

Miller, Carey D.

doi:10.1042/bj0200515

Cited by 11 publications

(6 citation statements)

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“…In the context of a spinning shell this might suggest that the shell recouples to the underlying star more quickly than in 4U 17284U -34 or 4U 17024U -429. Interestingly, 4U 1636 is also the only source to show significant pulsations at the sub-harmonic of the strongest oscillation frequency, and this has been interpreted as revealing the presence of a pair of antipodal hot spots (see Miller 1999a). These properties may be related and could, for example, indicate the presence of a stronger magnetic field in 4U 1636-53 than the other sources.…”

Section: Discussion and Summarymentioning

confidence: 97%

“…Oscillations at 580 Hz were discovered in thermonuclear bursts from 4U 1636-53 by Zhang et al (1996). More recently, Miller (1999a) has reported evidence during the rising phase of bursts of a significant modulation at half the 580 Hz frequency suggesting that 580 Hz is twice the neutron star spin frequency and that a pair of antipodal spots produce the oscillations. Here we focus on a burst from 4U 1636-53 which shows a unique decrease in the ≈ 580 Hz oscillation frequency.…”

Section: Evidence For Spin Downmentioning

confidence: 99%

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Spin-down of Pulsations in the Cooling Tail of an X-Ray Burst from 4U 1636−53

Strohmayer

1999

The Astrophysical Journal

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We report the discovery with the proportional counter array (PCA) onboard the Rossi X-ray Timing Explorer (RXTE) of a decrease in the frequency of X-ray brightness oscillations in the cooling tail of an X-ray burst from 4U 1636-53. This is the first direct evidence for a spin down of the pulsations seen during thermonuclear bursts. We find that the spin down episode is correlated with the appearance in this burst of an extended tail of emission with a decay timescale much longer than is seen in other bursts from 4U 1636-53 in the same set of observations. We present both time resolved energy and variability spectra during this burst and compare them with results from a second burst which shows neither a spin down episode nor an extended tail. A spectral evolution study of the "spin down" burst reveals a secondary signature of weak radius expansion, not seen in other bursts, and correlated with the spin down episode, which may indicate a secondary thermonuclear energy release. We interpret the spin down episode in the context of an angular momentum conserving shell, which is reexpanded and therefore spun down by an additional thermonuclear energy release which could also explain the extended X-ray tail.

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Section: Discussion and Summarymentioning

confidence: 97%

Section: Evidence For Spin Downmentioning

confidence: 99%

Spin-down of Pulsations in the Cooling Tail of an X-Ray Burst from 4U 1636−53

Strohmayer

1999

The Astrophysical Journal

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“…A. TIMES OF ARRIVAL, LIGHT CURVES, AND TABLES 199619971999200020042006200720102011 year 4U Note- Table 2 columns: (1) source name;…”

Section: Appendixmentioning

confidence: 99%

“…In addition to TBO candidates, we detect a few lowfrequency candidates and a large, but insignificant number of noise candidates (p = 1). Miller (1999) reported a significant signal at 290 Hz from the sum of 0.75-s intervals on the rise of five bursts. None of our noise candidates were close to 290 Hz.…”

Section: B13 4u 1636−536mentioning

confidence: 99%

A Uniform Search for Thermonuclear Burst Oscillations in the RXTE Legacy Data Set

Bilous

Watts

2019

ApJS

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We describe a blind uniform search for thermonuclear burst oscillations (TBOs) in the majority of Type-I bursts observed by RXTE (2118 bursts from 57 neutron stars). We examined 2-2002 Hz power spectra from the Fourier transform in sliding 0.5-2 s windows, using fine-binned light curves in 2-60 keV energy range. The significance of the oscillation candidates was assessed by simulations which took into account light curve variations, dead time and sliding time windows. Some of our sources exhibited multi-frequency variability at 15 Hz that cannot be readily removed with light-curve modeling and may have an astrophysical (non-TBO) nature. Overall, we found that the number and strength of potential candidates depends strongly on the parameters of the search. We found candidates from all previously known RXTE TBO sources, with pulsations that had been detected at similar frequencies in multiple independent time windows, and discovered TBOs from SAX J1810.8−2658. We could not confirm most previously-reported tentative TBO detections or identify any obvious candidates just below the detection threshold at similar frequencies in multiple bursts. We computed fractional amplitudes of all TBO candidates and placed upper limits on non-detections. Finally, for a few sources we noted small excess of candidates with powers comparable to fainter TBOs, but appearing in single independent time windows at random frequencies. At least some of these candidates may be noise spikes that appear interesting due to selection effects. The potential presence of such candidates calls for extra caution if claiming single-window TBO detections.

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“…1) Metabolites of azo-dye carcinogens bind covalently to specific soluble proteins in the rat liver (Miller & Miller, 1947;Sorof, Young, McCue & Fetterman, 1963). A basic azo-dye-binding protein has been isolated in apparently pure form and a small-molecular azo-dye-binding protein fraction has been substantially purified (Ketterer, RossMansell & Whitehead, 1967).…”

Section: Identification Of the Amino Acid Residues Thatmentioning

confidence: 99%