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In an X-ray pulsar, a neutron star accretes matter from a stellar companion through an accretion disk. The high magnetic field of the rotating neutron star disrupts the inner edge of the disc, funneling the gas to flow onto the magnetic poles on its surface. Hercules X-1 is in many ways the prototypical X-ray pulsar; it shows persistent X-ray emission and it resides with its companion HZ Her, a two-solar-mass star, at about 7~kpc from Earth1. Its emission varies on three distinct timescales2 the neutron star rotates every 1.2~seconds, it is eclipsed by its companion each 1.7~days, and the system exhibits a superorbital period of 35~days which has remained remarkably stable since its discovery3. Several lines of evidence point to the source of this variation as the precession of the accretion disc4,5, the precession of the neutron star6,7 or both8. Despite the many hints over the past fifty years, the precession of the neutron star itself has yet not been confirmed or refuted. We here present X-ray polarization measurements with the Imaging X-ray Polarimetry Explorer9 (IXPE) which probe the spin geometry of the neutron star. These observations provide direct evidence that the 35-day-period is set by the free precession of the neutron star crust, which has the important implication that its moment of inertia eigenvalues differ fractionally by a few parts per ten million10. Furthermore, we find indications that the basic spin geometry of the neutron star is altered by torques on timescale of a few hundred days.

The Galactic Center harbors diffuse X-ray emission co-spatial with giant molecular clouds and featuring hard X-ray spectra with a prominent fluorescent iron line at 6.4 keV [1–3]. These spectral properties are characteristic of the reflected emission from a neutral gas illuminated by X-rays. However, there are no persistent X-ray sources in that region that are bright enough to provide the required illumination level. Moreover, the observed diffuse emission is variable on time scales of years [4, 5], implying that the primary source of X-rays must be variable, too. The most exciting and far-reaching scenario is that a very powerful flare from the central supermassive black hole of the Milky Way, Sgr A*, provided the required flux of X-ray photons, when for a period shorter than a few years it became at least five orders of magnitude brighter than is typically observed today. Even if the primary emission was unpolarized, the reflected emission should be polarized in the direction perpendicular to the scattering plane with the degree of polarization being set by the scattering angle. Therefore, by measuring X-ray polarization one can infer the direction towards the primary source and, simultaneously, the mutual positions in space of the source and the cloud [6]. Here, we report the detection of X-ray polarization from the Galactic Center region obtained by the recently launched Imaging X-ray Polarimetry Explorer (IXPE) mission. For a large region where Chandra and XMM-Newton identify spectral signatures of the reflection, IXPE measures a polarization degree of 31% ± 11% with a polarization angle -48° ± 11° for the scattered continuum. The latter corroborates the conjecture that Sgr A* is the primary source of illuminating photons, while the former implies that some 200 years ago our Galactic Center hosted an extremely bright active galactic nucleus, on par with the ones found in Seyfert galaxies, though only for a short time.

Using observations of X-ray pulsar Her X-1 by the Imaging X-ray Polarimetry Explorer, we report on a highly significant detection of the polarization signal from an accreting neutron star. The observed degree of the linear polarization of ∼ 10% is found to be far below theoretical expectations for this object, and stays low throughout the spin cycle of the pulsar. Both the polarization degree and the angle exhibit variability with pulse phase, which allowed us to measure the pulsar spin position angle and magnetic obliquity of the neutron star, which is an essential step towards detailed modeling of the intrinsic emission of X-ray pulsars. Combining our results with the optical polarimetric data, we find that the spin axis of the neutron star and the angular momentum of the binary orbit are misaligned by at least ∼20 deg, which is a strong argument in support of the models explaining stability of the observed super-orbital variability with the precession of the neutron star.

Preharvest treatment with 400 ppm aminoethoxyvinylglycine (AVG) delayed the ripening of ‘Bartlett’ pears kept at 20°C. The effect was not uniform, with the delay in ripening ranging from a few to 112 days. Prolonged storage at 20° was accompanied by a relatively steady, low level of respiration, gradual degreening, and partial suppression of the eventual climacteric. The combined effect of AVG treatment and prolonged ‘nonripening’ storage at 20° led to a marked attentuation of the production of 4 readily measurable volatiles including methyl-, ethyl-, and hexylacetate as identified by cochromatography and combined gas chromatography–mass spectrometry. Surprisingly, prolonged storage resulted in a much increased production of 2 other volatile fractions when AVG inhibition was reversed by C2H4 treatment. The emanation of all measured volatiles was closely coincident with the climacteric peak. These observations confirm prior reports of disuniform effects of preharvest AVG treatment and reveal that metabolic transitions during prolonged, nonripening storage may have adverse effects on fruit quality.

Isolated mitochondria were maintained metabolically active and coupled, i.e., capable of respiratory control, for several hours at 25°C. An increase in respiratory control generally occurred during the first 4-8 hr of incubation followed thereafter by a decline. Longevity is a dynamic function as evidenced by its dependency on substrate and cofactors, thiamine pyrophosphate, in particular. Magnesium was also essential to longevity; coenzyme A, bovine serum albumin, and reducing agents were not. The findings are discussed in terms of cytoplasmic-mitochondrial interrelationships and mitochondrial autonomy.

Application of 400 ppm aminoethoxyvinylglycine (AVG) to pear trees 6 and 2 weeks before harvest resulted in marked but variable inhibition of postharvest ripening at 20°C. AVG amplified the usual nonuniformity in the initiation of ripening exhibited by freshly harvested fruit. Prolonged storage of the fruit at 0 to 2°c counteracted the inhibitory effects with resultant rapid and uniform ripening upon transfer to 20°c. However, a physiological nonuniformity as reflected by wide differences in internal C2H4 concentration persisted well beyond the time when threshold levels for the initiation of ripening had been reached by all fruit. Probable relationships between AVG effects, cold storage, and C2H4 are illustrated diagrammatically.