An Elegy Upon S. W. R.

King, Henry; Saintsbury, George

doi:10.1093/oseo/instance.00007067

Cited by 52 publications

(112 citation statements)

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“…Like follicles in earlier stages, these post-collapse follicles show a relatively large current entering their most anterior accessible point. By this stage, however, the anterior pole current enters a region over the shrunken remnants of the nurse cells, which are supposed to be disconnected from the oocyte (16,17). Moreover, as before, less intense currents leave most of the rest of the oocyte.…”

Section: Vitellogenic Folliflesmentioning

confidence: 82%

Large electrical currents traverse developing Ceropia follicles

Jaffe

Woodruff

1979

Proc. Natl. Acad. Sci. U.S.A.

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An intense (up to 20 M&A/cm2) steady electrical current enters the anterior or nurse cell end of the growing follicle (or oocyte-nurse cell complex) of the Cecropia moth and is balanced by a more diffuse current leaving elsewhere. In late growth stages, the total transfollicular current is about 100 nA. Moreover, a separate small current, of about 1 nA, seems to leave the furrow between the oocyte and the nurse cells. After the nurse cells collapse, but before shell formation, the transfollicular current is redistributed so that a second relatively localized inward current appears at the posterior pole of the follicle. Thus, at this later stage currents enter both poles of the follicle and leave its sides. Previous measurements, with intracellular microelectrodes, seem to imply a very large (order of 1000 nA) back current across the cytoplasmic bridge between the oocyte and nurse cells. A simple model is presented that attributes the apparent bridge current, and the more directly measured transfollicular and furrow currents, to the action of an ion pump lying within the nurse cell face of the furrow membrane.

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Section: Vitellogenic Folliflesmentioning

confidence: 82%

Large electrical currents traverse developing Ceropia follicles

Jaffe

Woodruff

1979

Proc. Natl. Acad. Sci. U.S.A.

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“…Centrin is a subunit of some inner dynein arms (7). LC4 is a subunit of outer dynein arms (8). The presence of multiple calcium-binding proteins each associated with a discrete axonemal structure suggests that there are multiple sites of calcium control in the flagellum.…”

Section: Discussionmentioning

confidence: 99%

“…calmodulin (5,6), centrin/caltractin (7), and dynein light chain 4 (see Ref. 8 and see below), have been identified within the axoneme, but their precise functions in Ca 2ϩ -mediated flagellar behavior have not yet been clearly defined. Given the complexity of the axoneme and the likely need to modulate the activity of multiple axonemal structures to achieve a coordinated change in waveform in response to changes in Ca 2ϩ concentration, it is probable that the axoneme contains additional Ca 2ϩ -binding proteins.…”

mentioning

confidence: 99%

“…The generation of symmetrical bends during photoshock requires the outer dynein arms (9,10), suggesting that the outer arms are regulated by Ca 2ϩ . One outer dynein arm light chain, LC4, 1 is a Ca 2ϩ -binding protein, and it has been hypothesized that this subunit may have a role in mediating outer arm function during photoshock (8); however, there currently is no experimental evidence in support of such a role for LC4.…”

mentioning

confidence: 99%

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DC3, the Smallest Subunit of the Chlamydomonas Flagellar Outer Dynein Arm-docking Complex, Is a Redox-sensitive Calcium-binding Protein

Casey

Yagi

Kamiya

et al. 2003

Journal of Biological Chemistry

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“…Hawking, King and McCarthy (1975) have suggested a topology determining the causal, differential and conformal structure of space-time, replacing a suggestion of Zeeman (1964). Zeeman had noted that the group preserving time-ordering along paths of free particles is the Poincare group and scale invariance.…”

Section: Pathologiesmentioning

confidence: 99%

47. Cosmology

Longair¹

1976

Trans. Int. Astron. Union

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A. H 0 and i2A major procedural advance in the determination of the H 0 and J2 has been that the problem is now being attacked from many different points of view and to some extent the observations are converging on preferred values of H 0 and £2 (£2 = density parameter = 8jrGp 0 /3H 0 where p 0 is the mean density of matter in the Universe and H 0 is the Hubble constant; £2 = 2q 0 where q 0 is the deceleration parameter). The classical approaches through the redshift-magnitude relation for the most massive galaxies in clusters suggest a value of H 0 = 60 km s _ I Mpc (see the review by Tammann in IAU Symp. 63).The classical approach to the determination of £2 is through the extension of the redshift-magnitude relation to large redshifts and the major contributions have been made by Sandage and by Gunn and Oke. Of particular importance has been the use of the multichannel scanner on the 200-in. telescope to determine the absolute spectra of galaxies. Two important advances are:(i) the redshift range 0.3 to 0.5 has been filled out by the addition of about 17 new galaxies which are the brightest members of clusters to the M-Z plot;(ii) the problem of K-corrections is eliminated since the absolute spectrum of each galaxy is measured. One result of immediate importance is that 3C295, which is at a redshift of 0.461 and which up till recently was the only object at such a large redshift, appears to be intrinsically brighter than other first ranking galaxies in clusters. Gunn and Oke (Astrophys. J. 195, 255, 1975) find that the best fitting value of q 0 is small, q 0 = 0.31 ±0.68 (3C295 included) or q 0 = -0 . 1 5 ± 0.54 (3C295 excluded) without making any allowance for cosmological evolution. Formally, if allowance is made for the evolution of the luminosity of the most massive galaxies in clusters, the best fit value of q 0 is negative, q 0 = -0.43 ± 0.54 (3C295 included) or q 0 = -1.27 ± 0.62 (3C295 excluded), i.e. the Universe is accelerating. A literal interpretation of this result suggests that the cosmological constant A is non-zero. However, what has become increasingly apparent even with the much improved data-base, is the great sensitivity of q 0 to very small corrections. Sandage's approach has been to investigate all possible correlations between the properties of massive galaxies in clusters and cluster membership and to calibrate out these effects. Serious problems remain, however, with very small corrections which depend upon the astrophysical evolution of massive galaxies in clusters. The problem of estimating the 'static' evolution of a massive galaxy in a cluster has already been mentioned. There is also the question of how the most massive galaxies in clusters form. If, as seems plausible, they are massive because matter in the cluster has nowhere else to fall, there could well be significant changes in their luminosities over cosmological time-scales. Recently Ostriker and Tremaine have discussed the problem of the central massive galaxy disrupting and 'swallowing' spiral galaxies in the cluster....

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An Elegy Upon S. W. R.

Cited by 52 publications

References 0 publications

Large electrical currents traverse developing Ceropia follicles

Large electrical currents traverse developing Ceropia follicles

DC3, the Smallest Subunit of the Chlamydomonas Flagellar Outer Dynein Arm-docking Complex, Is a Redox-sensitive Calcium-binding Protein

47. Cosmology

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