141 research outputs found
Morgan's canon, Garner's phonograph, and the evolutionary origins of language and reason
`Morgan's canon' is a rule for making inferences from animal behaviour about animal minds, proposed in 1892 by the Bristol geologist and zoologist C. Lloyd Morgan, and celebrated for promoting scepticism about the reasoning powers of animals. Here I offer a new account of the origins and early career of the canon. Built into the canon, I argue, is the doctrine of the Oxford philologist F. Max Mu llerian origins of the canon in turn illuminates a number of changes in Morgan's position between 1892 and 1894. I explain these changes as responses to the work of the American naturalist R. L. Garner. Where Morgan had a rule for interpreting experiments with animals, Garner had an instrument for doing them: the Edison cylinder phonograph. Using the phonograph, Garner claimed to provide experimental proof that animals indeed spoke and reasoned
So many free lunches: Why we should not try to be excellent. "GOOD ENOUGH: The tolerance for mediocrity in nature and society" (310pp. Harvard University Press. ÂŁ20 (US $28.95), Daniel S. Milo)
Genetic Determinism in the Genetics Curriculum: An Exploratory Study of the Effects of Mendelian and Weldonian Emphases
Twenty-first century biology rejects genetic determinism, yet an exaggerated view of the power of genes in the making of bodies and minds remains a problem. What accounts for such tenacity? This article reports an exploratory study suggesting that the common reliance on Mendelian examples and concepts at the start of teaching in basic genetics is an eliminable source of determinism. Undergraduate students who attended a standard âMendelian approachâ university course in introductory genetics on average showed no change in their determinist views about genes. By contrast, students who attended an alternative course which, inspired by the work of a critic of early Mendelism, W. F. R. Weldon (1860-1906), replaced an emphasis on Mendelâs peas with an emphasis on developmental contexts and their role in bringing about phenotypic variability, were less determinist about genes by the end of teaching. Improvements in both the new Weldonian curriculum and the study design are in view for the future
Of Lice and Men: Charles Darwin, Henry Denny and the Evidence for the Human Races as Varieties or Species
Charles Darwin never doubted the common ancestry of the human races. But he was open-minded about whether the races might nevertheless be so different from each other that they ought to be classified not as varieties of one species but as distinct species. He pondered this varieties-or-species question on and off for decades, from his time aboard the Beagle through to the publication of the Descent of Man. A constant throughout was his concern with something that he first learned on the Beagle voyage and that, on the face of it, seemed to favour the species ranking: the different races, he was told, play host to distinct species of lice. This paper reconstructs the long run of Darwin's reflections and interactions on race, lice and history, using his extended correspondence with Henry Denny â curator of the scientific collections of the Leeds Philosophical and Literary Society, and Britain's leading expert in the natural history of lice â as a window onto the social world whose imprint is everywhere in the pages of the Descent
Confronting a solar irradiance reconstruction with solar and stellar data
Context. A recent paper by Shapiro and colleagues (2011, A&A, 529, A67) reconstructs spectral and total irradiance variations of the Sun during the holocene.
Aims. In this note, we comment on why their methodology leads to large (0.5%) variations in the solar TSI on century-long time scales, in stark contrast to other reconstructions which have âČ 0.1% variations.
Methods. We examine the amplitude of the irradiance variations from the point of view of both solar and stellar data.
Results. Shapiro et al.âs large amplitudes arise from differences between the irradiances computed from models A and C of Fontenla and colleagues, and from their explicit assumption that the radiances of the quiet Sun vary with the cosmic ray modulation potential. We suggest that the upper photosphere, as given by model A, is too cool, and discuss relative contributions of local vs. global dynamos to the magnetism and irradiance of the quiet Sun. We compare the slow (\u3e22 yr) components of the irradiance reconstructions with secular changes in stellar photometric data that span 20 years or less, and find that the Sun, if varying with such large amplitudes, would still lie within the distribution of stellar photometric variations measured over a 10â20 year period. However, the stellar time series are individually too short to see if the reconstructed variations will remain consistent with stellar variations when observed for several decades more.
Conclusions. By adopting model A, Shapiro et al. have over-estimated quiet-Sun irradiance variations by about a factor of two, based upon a re-analysis of sub-mm data from the James Clerk Maxwell telescope. But both estimates are within bounds set by current stellar data. It is therefore vital to continue accurate photometry of solar-like stars for at least another decade, to reveal secular and cyclic variations on multi-decadal time scales of direct interest to the Sun
Fine structure of the chromospheric activity in Solar-type stars - The Halpha Line
A calibration of H-alpha as both a chromospheric diagnostic and an age
indicator is presented, complementing the works previously done on this subject
(Herbig 1985, Pasquini & Pallavicini 1991. The chromospheric diagnostic was
built with a statistically significant sample, covering nine years of
observations, and including 175 solar neighborhood stars. Regarding the age
indicator, the presence of stars for which very accurate ages are determined,
such as those belonging to clusters and kinematic groups, lends confidence to
our analysis. We also investigate the possibility that stars of the same age
might have gone through different tracks of chromospheric decay, identifying -
within the same age range - effects of metallicity and mass. These parameters,
however, as well as age, seem to be significant only for dwarf stars, losing
their meaning when we analyze stars in the subgiant branch. This result
suggests that, in these evolved stars, the emission mechanism cannot be
magnetohydrodynamical in nature, in agreement with recent models (Fawzy et al.
2002c, and references therein). The Sun is found to be a typical star in its
H-alpha chromospheric flux, for its age, mass and metallicity. As a byproduct
of this work, we developed an automatic method to determine temperatures from
the wings of H-alpha, which means the suppression of the error inherent to the
visual procedure used in the literature.Comment: 10 pages, 10 figures, accepted for publication in Astronomy &
Astrophysics. Nature of replacement: match astro-ph and ADS title (greek
letter
Characterising stellar micro-variability for planetary transit searches
Copyright © The European Southern Observatory (ESO)A method for simulating light curves containing stellar micro-variability for a range of spectral types and ages is presented. It is based on parameter-by-parameter scaling of a multi-component fit to the solar irradiance power spectrum (based on VIRGO/PMO6 data), and scaling laws derived from ground based observations of various stellar samples.
A correlation is observed in the Sun between the amplitude of the power spectrum on long (weeks) timescales and the BBSO Ca II K-line index of chromospheric activity. On the basis of this evidence, the chromospheric activity level, predicted from rotation period and B-V colour estimates according to the relationship first introduced by Noyes (1983) and Noyes et al. (1984), is used to predict the variability power on weeks time scales. The rotation period is estimated on the basis of a fit to the distribution of rotation period versus B-V observed in the Hyades and the Skumanich (1972) spin-down law. The characteristic timescale of the variability is also scaled according to the rotation period.
This model is used to estimate the impact of the target star spectral type and age on the detection capability of space based transit searches such as Eddington and Kepler. K stars are found to be the most promising targets, while the performance drops significantly for stars earlier than G and younger than 2.0 Gyr. Simulations also show that Eddington should detect terrestrial planets orbiting solar-age stars in most of the habitable zone for G2 types and all of it for K0 and K5 types
Photospheric activity, rotation, and star-planet interaction of the planet-hosting star CoRoT-6
The CoRoT satellite has recently discovered a hot Jupiter that transits
across the disc of a F9V star called CoRoT-6 with a period of 8.886 days. We
model the photospheric activity of the star and use the maps of the active
regions to study stellar differential rotation and the star-planet interaction.
We apply a maximum entropy spot model to fit the optical modulation as observed
by CoRoT during a uninterrupted interval of about 140 days. Photospheric active
regions are assumed to consist of spots and faculae in a fixed proportion with
solar-like contrasts. Individual active regions have lifetimes up to 30-40
days. Most of them form and decay within five active longitudes whose different
migration rates are attributed to the stellar differential rotation for which a
lower limit of \Delta \Omega / \Omega = 0.12 \pm 0.02 is obtained. Several
active regions show a maximum of activity at a longitude lagging the
subplanetary point by about 200 degrees with the probability of a chance
occurrence being smaller than 1 percent. Our spot modelling indicates that the
photospheric activity of CoRoT-6 could be partially modulated by some kind of
star-planet magnetic interaction, while an interaction related to tides is
highly unlikely because of the weakness of the tidal force.Comment: 9 pages, 7 figures, accepted to Astronomy & Astrophysic
Patterns of photometric and chromospheric variation among Sun-like stars: A 20-year perspective
We examine patterns of variation of 32 primarily main sequence stars,
extending our previous 7-12 year time series to 13-20 years by combining b, y
data from Lowell Observatory with similar data from Fairborn Observatory.
Parallel chromospheric Ca II H and K emission data from the Mount Wilson
Observatory span the entire interval. The extended data strengthen the
relationship between chromospheric and photometric variation derived
previously. Twenty-seven stars are deemed variable. On a year-to-year timescale
young active stars become fainter when their Ca II emission increases while
older less active stars such as the Sun become brighter when their Ca II
emission increases. The Sun's total irradiance variation, scaled to the b and y
filter photometry, still appears to be somewhat smaller than stars in our
limited sample with similar mean chromospheric activity, but we now regard this
discrepancy as probably due mainly to our limited stellar sampl
Rotation of planet-harbouring stars
The rotation rate of a star has important implications for the detectability,
characterisation and stability of any planets that may be orbiting it. This
chapter gives a brief overview of stellar rotation before describing the
methods used to measure the rotation periods of planet host stars, the factors
affecting the evolution of a star's rotation rate, stellar age estimates based
on rotation, and an overview of the observed trends in the rotation properties
of stars with planets.Comment: 16 pages, 4 figures: Invited review to appear in 'Handbook of
Exoplanets', Springer Reference Works, edited by Hans J. Deeg and Juan
Antonio Belmont
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