Environment

@book{young1938the8,
    author = "Young, J. Z",
    title = "The Evolution of the Nervous System and of the Relationship of Organism and Environment, in de Beer, G. R., ed., Evolution",
    year = "1938",
    publisher = "Essays on Aspects of Evolutionary Biology, Presented to Professor E.S. Goodrich on his 70th Birthday: Oxford, Claredon Press, p. 179-204",
    note = "talkorigins\_source = {true}; raw\_reference = {Young, J. Z., 1938, The Evolution of the Nervous System and of the Relationship of Organism and Environment, in de Beer, G. R., ed., Evolution: Essays on Aspects of Evolutionary Biology, Presented to Professor E.S. Goodrich on his 70th Birthday: Oxford, Claredon Press, p. 179-204.}"
}

@misc{ayala1968genotype1,
    author = "Ayala, F. J",
    title = "Genotype, environment, and population numbers",
    year = "1968",
    howpublished = "Science, v. 162, p. 1453-1459",
    note = "talkorigins\_source = {true}; raw\_reference = {Ayala, F. J., 1968, Genotype, environment, and population numbers: Science, v. 162, p. 1453-1459.}"
}

@book{drake1968evolution2,
    author = "Drake, E. T",
    title = "Evolution and environment",
    year = "1968",
    publisher = "New Haven, Connecticut, Yale University Press, 478 p",
    note = "talkorigins\_source = {true}; raw\_reference = {Drake, E. T., 1968, Evolution and environment: New Haven, Connecticut, Yale University Press, 478 p.}"
}

@article{bernard1970evolution,
    author = "Bernard, E.A.",
    title = "Evolution and environment",
    year = "1970",
    journal = "Palaeogeography, Palaeoclimatology, Palaeoecology",
    url = "https://doi.org/10.1016/0031-0182(70)90095-7",
    doi = "10.1016/0031-0182(70)90095-7",
    number = "3",
    openalex = "W2322098789",
    pages = "277-278",
    volume = "7"
}

@misc{fuller1974chemistry3,
    author = "Fuller, E. C",
    title = "Chemistry and Man's Environment",
    year = "1974",
    howpublished = "Boston, Houghton Mifflin",
    note = "talkorigins\_source = {true}; raw\_reference = {Fuller, E. C., 1974, Chemistry and Man's Environment: Boston, Houghton Mifflin.}"
}

@book{hallam1975jurassic4,
    author = "Hallam, A",
    title = "Jurassic Environments",
    year = "1975",
    publisher = "Cambridge, Cambridge University Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Hallam, A., 1975, Jurassic Environments: Cambridge, Cambridge University Press.}"
}

@book{schmidtnielsen1979animal6,
    author = "Schmidt-Nielsen, K",
    title = "Animal Physiology, Adaptation and Environment",
    year = "1979",
    publisher = "Cambridge, Cambridge University Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Schmidt-Nielsen, K., 1979, Animal Physiology, Adaptation and Environment: Cambridge, Cambridge University Press.}"
}

@book{panchen1980the5,
    author = "Panchen, A. L",
    title = "The Terrestrial Environment and the Origin of Land Vertebrates",
    year = "1980",
    publisher = "New York, Academic Press",
    note = "talkorigins\_source = {true}; raw\_reference = {Panchen, A. L., 1980, The Terrestrial Environment and the Origin of Land Vertebrates: New York, Academic Press.}"
}

Studies of spatial variation in the environment have primarily focused on how genetic variation can be maintained. Many one-locus genetic models have addressed this issue, but, for several reasons, these models are not directly applicable to quantitative (polygenic) traits. One reason is that for continuously varying characters, the evolution of the mean phenotype expressed in different environments (the norm of reaction) is also of interest. Our quantitative genetic models describe the evolution of phenotypic response to the environment, also known as phenotypic plasticity (Gause, 1947), and illustrate how the norm of reaction (Schmalhausen, 1949) can be shaped by selection. These models utilize the statistical relationship which exists between genotype-environment interaction and genetic correlation to describe evolution of the mean phenotype under soft and hard selection in coarse-grained environments. Just as genetic correlations among characters within a single environment can constrain the response to simultaneous selection, so can a genetic correlation between states of a character which are expressed in two environments. Unless the genetic correlation across environments is ± 1, polygenic variation is exhausted, or there is a cost to plasticity, panmictic populations under a bivariate fitness function will eventually attain the optimum mean phenotype for a given character in each environment. However, very high positive or negative correlations can substantially slow the rate of evolution and may produce temporary maladaptation in one environment before the optimum joint phenotype is finally attained. Evolutionary trajectories under hard and soft selection can differ: in hard selection, the environments with the highest initial mean fitness contribute most individuals to the mating pool. In both hard and soft selection, evolution toward the optimum in a rare environment is much slower than it is in a common one. A subdivided population model reveals that migration restriction can facilitate local adaptation. However, unless there is no migration or one of the special cases discussed for panmictic populations holds, no geographical variation in the norm of reaction will be maintained at equilibrium. Implications of these results for the interpretation of spatial patterns of phenotypic variation in natural populations are discussed.

@article{doi101111j155856461985tb00391x,
    author = "Via, Sara and Lande, Russell",
    title = "GENOTYPE-ENVIRONMENT INTERACTION AND THE EVOLUTION OF PHENOTYPIC PLASTICITY",
    year = "1985",
    journal = "Evolution",
    abstract = "Studies of spatial variation in the environment have primarily focused on how genetic variation can be maintained. Many one-locus genetic models have addressed this issue, but, for several reasons, these models are not directly applicable to quantitative (polygenic) traits. One reason is that for continuously varying characters, the evolution of the mean phenotype expressed in different environments (the norm of reaction) is also of interest. Our quantitative genetic models describe the evolution of phenotypic response to the environment, also known as phenotypic plasticity (Gause, 1947), and illustrate how the norm of reaction (Schmalhausen, 1949) can be shaped by selection. These models utilize the statistical relationship which exists between genotype-environment interaction and genetic correlation to describe evolution of the mean phenotype under soft and hard selection in coarse-grained environments. Just as genetic correlations among characters within a single environment can constrain the response to simultaneous selection, so can a genetic correlation between states of a character which are expressed in two environments. Unless the genetic correlation across environments is ± 1, polygenic variation is exhausted, or there is a cost to plasticity, panmictic populations under a bivariate fitness function will eventually attain the optimum mean phenotype for a given character in each environment. However, very high positive or negative correlations can substantially slow the rate of evolution and may produce temporary maladaptation in one environment before the optimum joint phenotype is finally attained. Evolutionary trajectories under hard and soft selection can differ: in hard selection, the environments with the highest initial mean fitness contribute most individuals to the mating pool. In both hard and soft selection, evolution toward the optimum in a rare environment is much slower than it is in a common one. A subdivided population model reveals that migration restriction can facilitate local adaptation. However, unless there is no migration or one of the special cases discussed for panmictic populations holds, no geographical variation in the norm of reaction will be maintained at equilibrium. Implications of these results for the interpretation of spatial patterns of phenotypic variation in natural populations are discussed.",
    url = "https://doi.org/10.1111/j.1558-5646.1985.tb00391.x",
    doi = "10.1111/j.1558-5646.1985.tb00391.x",
    openalex = "W2014857933",
    references = "doi101001jama195002910300087029, doi101016s0065266008600486, doi101086281736, doi101086281792, doi101111j155856461979tb04694x, doi101111j155856461980tb04817x, doi101111j155856461981tb04864x, doi101111j155856461983tb00236x, doi1023071936778, doi1023072407630, doi1023072527750"
}

@misc{weiss1989lower7,
    author = "Weiss, A. F. and Semikhatov, M. A",
    title = "Lower Riphean Omakhta microfossil association of East Siberia",
    year = "1989",
    howpublished = "composition and formation environments [in Russian]: Izvestia Akadamie Nauk SSSR Series Geol., v. 5, p. 36-54",
    note = "talkorigins\_source = {true}; raw\_reference = {Weiss, A. F., and Semikhatov, M. A., 1989, Lower Riphean Omakhta microfossil association of East Siberia: composition and formation environments [in Russian]: Izvestia Akadamie Nauk SSSR Series Geol., v. 5, p. 36-54.}"
}

@article{doi1023071485903,
    author = "Berggren, William A. and Tsuchi, Ryiuchi and Ingle, James C.",
    title = "Pacific Neogene: Environment, Evolution and Events",
    year = "1993",
    journal = "Micropaleontology",
    url = "https://doi.org/10.2307/1485903",
    doi = "10.2307/1485903",
    openalex = "W1538093094"
}

@incollection{crossref1994evolution,
    title = "Evolution and environment",
    year = "1994",
    booktitle = "New Views on an Old Planet",
    url = "https://doi.org/10.1017/cbo9781139174114.026",
    doi = "10.1017/cbo9781139174114.026",
    openalex = "W2483247563",
    pages = "348-370"
}

We study dark matter halo density profiles in a high-resolution N-body simulation of a LCDM cosmology. Our statistical sample contains,5000 haloes in the range 10 11 10 14 h 21 M (Y and the resolution allows a study of subhaloes inside host haloes. The profiles are parametrized by an NFW form with two parameters, an inner radius r s and a virial radius R vir, and we define the halo concentration c vir; R vir ar s X First, we find that, for a given halo mass, the redshift dependence of the median concentration is c vir G 1 1 z 21 X This corresponds to r s z, constantY and is contrary to earlier suspicions that c vir does not vary much with redshift. The implications are that high-redshift galaxies are predicted to be more extended and dimmer than expected before. Secondly, we find that the scatter in halo profiles is large, with a 1s Dlog c vir 0X18 at a given mass, corresponding to a scatter in maximum rotation velocities of DV max aV max 0X12X We discuss implications for modelling the TullyFisher relation, which has a smaller reported intrinsic scatter. Thirdly, subhaloes and haloes in dense environments tend to be more concentrated than isolated haloes, and show a larger scatter. These results suggest that c vir is an essential parameter for the theory of galaxy modelling, and we briefly discuss implications for the universality of the Tully Fisher relation, the formation of low surface brightness galaxies, and the origin of the Hubble sequence. We present an improved analytic treatment of halo formation that fits the measured relations between halo parameters and their redshift dependence, and can thus serve semi-analytic studies of galaxy formation.

@article{doi101046j13658711200104068x,
    author = "Bullock, James S. and Kolatt, Tsafrir and Sigad, Yair and Somerville, Rachel S. and Kravtsov, Andrey V. and Klypin, A. A. and Primack, Joel R. and Dekel, Avishai",
    title = "Profiles of dark haloes: evolution, scatter and environment",
    year = "2001",
    journal = "Monthly Notices of the Royal Astronomical Society",
    abstract = "We study dark matter halo density profiles in a high-resolution N-body simulation of a LCDM cosmology. Our statistical sample contains,5000 haloes in the range 10 11 10 14 h 21 M (Y and the resolution allows a study of subhaloes inside host haloes. The profiles are parametrized by an NFW form with two parameters, an inner radius r s and a virial radius R vir, and we define the halo concentration c vir; R vir ar s X First, we find that, for a given halo mass, the redshift dependence of the median concentration is c vir G 1 1 z 21 X This corresponds to r s z, constantY and is contrary to earlier suspicions that c vir does not vary much with redshift. The implications are that high-redshift galaxies are predicted to be more extended and dimmer than expected before. Secondly, we find that the scatter in halo profiles is large, with a 1s Dlog c vir 0X18 at a given mass, corresponding to a scatter in maximum rotation velocities of DV max aV max 0X12X We discuss implications for modelling the TullyFisher relation, which has a smaller reported intrinsic scatter. Thirdly, subhaloes and haloes in dense environments tend to be more concentrated than isolated haloes, and show a larger scatter. These results suggest that c vir is an essential parameter for the theory of galaxy modelling, and we briefly discuss implications for the universality of the Tully Fisher relation, the formation of low surface brightness galaxies, and the origin of the Hubble sequence. We present an improved analytic treatment of halo formation that fits the measured relations between halo parameters and their redshift dependence, and can thus serve semi-analytic studies of galaxy formation.",
    url = "https://doi.org/10.1046/j.1365-8711.2001.04068.x",
    doi = "10.1046/j.1365-8711.2001.04068.x",
    openalex = "W2023344562",
    references = "doi101046j13658711199801227x, doi101086152650, doi101086157753, doi101086170483, doi101086177173, doi101086304888, doi101086305262, doi101093mnras1833341, doi101093mnras2623627, openalexw3100110286"
}

@article{doi101016jibmb200309002,
    author = "Mans, Ben J. and Neitz, A.W.H.",
    title = "Adaptation of ticks to a blood-feeding environment: evolution from a functional perspective",
    year = "2004",
    journal = "Insect Biochemistry and Molecular Biology",
    url = "https://doi.org/10.1016/j.ibmb.2003.09.002",
    doi = "10.1016/j.ibmb.2003.09.002",
    openalex = "W2161609934",
    references = "doi1010079783642866593, doi1010160047248491900698, doi101016s0968000498013358, doi101042bj3180001, doi101074jbcr000003200, doi101126science28754612204, doi101126science29054941151, doi101146annurevbi49070180003113, openalexw1511493290, openalexw1517554598"
}

@book{openalexw1525648878,
    author = "Deeming, D. Charles",
    title = "Reptilian Incubation: Environment, Evolution and Behaviour",
    year = "2004",
    url = "https://openalex.org/W1525648878",
    openalex = "W1525648878"
}

We explore the simple inter-relationships between mass, star formation rate, and environment in the SDSS, zCOSMOS, and other deep surveys. We take a purely empirical approach in identifying those features of galaxy evolution that are demanded by the data and then explore the analytic consequences of these. We show that the differential effects of mass and environment are completely separable to z ~ 1, leading to the idea of two distinct processes of "mass quenching" and "environment quenching." The effect of environment quenching, at fixed over-density, evidently does not change with epoch to z ~ 1 in zCOSMOS, suggesting that the environment quenching occurs as large-scale structure develops in the universe, probably through the cessation of star formation in 30%-70% of satellite galaxies. In contrast, mass quenching appears to be a more dynamic process, governed by a quenching rate. We show that the observed constancy of the Schechter M* and α_s for star-forming galaxies demands that the quenching of galaxies around and above M* must follow a rate that is statistically proportional to their star formation rates (or closely mimic such a dependence). We then postulate that this simple mass-quenching law in fact holds over a much broader range of stellar mass (2 dex) and cosmic time. We show that the combination of these two quenching processes, plus some additional quenching due to merging naturally produces (1) a quasi-static single Schechter mass function for star-forming galaxies with an exponential cutoff at a value M* that is set uniquely by the constant of proportionality between the star formation and mass quenching rates and (2) a double Schechter function for passive galaxies with two components. The dominant component (at high masses) is produced by mass quenching and has exactly the same M* as the star-forming galaxies but a faint end slope that differs by Δα_s ~ 1. The other component is produced by environment effects and has the same M* and α_s as the star-forming galaxies but an amplitude that is strongly dependent on environment. Subsequent merging of quenched galaxies will modify these predictions somewhat in the denser environments, mildly increasing M* and making α_s slightly more negative. All of these detailed quantitative inter-relationships between the Schechter parameters of the star-forming and passive galaxies, across a broad range of environments, are indeed seen to high accuracy in the SDSS, lending strong support to our simple empirically based model. We find that the amount of post-quenching "dry merging" that could have occurred is quite constrained. Our model gives a prediction for the mass function of the population of transitory objects that are in the process of being quenched. Our simple empirical laws for the cessation of star formation in galaxies also naturally produce the "anti-hierarchical" run of mean age with mass for passive galaxies, as well as the qualitative variation of formation timescale indicated by the relative α-element abundances.

@article{doi1010880004637x7211193,
    author = "Peng, Yingjie and Lilly, S. J. and Kovač, Katarina and Bolzonella, M. and Pozzetti, L. and Renzini, A. and Zamorani, G. and Ilbert, O. and Knobel, C. and Iovino, A. and Maier, C. and Cucciati, O. and Tasca, Lidia and Carollo, C. Marcella and Silverman, John and Kampczyk, P. and de Ravel, L. and Sanders, D. B. and Scoville, Nicholas and Contini, T. and Mainieri, V. and Scodeggio, M. and Kneib, Jean‐Paul and Fèvre, O. Le and Bardelli, S. and Bongiorno, A. and Caputi, K. I. and Coppa, G. and de la Torre, Sylvain and Franzetti, P. and Garilli, B. and Lamareille, Fabrice and Borgne, Jean-Francois Le and Brun, Vincent Le and Mignoli, M. and Montero, Enrique Perez and Pelló, R. and Ricciardelli, E. and Tanaka, M. and Tresse, L. and Vergani, D. and Welikala, Niraj and Zucca, E. and Oesch, Pascal A. and Abbas, U. and Barnes, Luke A. and Bordoloi, Rongmon and Bottini, D. and Cappi, A. and Cassata, P. and Cimatti, Andrea and Fumana, M. and Hasinger, G. and Koekemoer, Anton M. and Leauthaud, Alexei and Maccagni, Dario and Marinoni, C. and McCracken, H. J. and Memeo, Pierdomenico and Meneux, B. and Nair, Preethi and Porciani, C. and Presotto, V. and Scaramella, R.",
    title = "MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION IN SDSS AND zCOSMOS AND THE ORIGIN OF THE SCHECHTER FUNCTION",
    year = "2010",
    journal = "The Astrophysical Journal",
    abstract = {We explore the simple inter-relationships between mass, star formation rate, and environment in the SDSS, zCOSMOS, and other deep surveys. We take a purely empirical approach in identifying those features of galaxy evolution that are demanded by the data and then explore the analytic consequences of these. We show that the differential effects of mass and environment are completely separable to z \textasciitilde\ 1, leading to the idea of two distinct processes of "mass quenching" and "environment quenching." The effect of environment quenching, at fixed over-density, evidently does not change with epoch to z \textasciitilde\ 1 in zCOSMOS, suggesting that the environment quenching occurs as large-scale structure develops in the universe, probably through the cessation of star formation in 30\%-70\% of satellite galaxies. In contrast, mass quenching appears to be a more dynamic process, governed by a quenching rate. We show that the observed constancy of the Schechter M* and α\_s for star-forming galaxies demands that the quenching of galaxies around and above M* must follow a rate that is statistically proportional to their star formation rates (or closely mimic such a dependence). We then postulate that this simple mass-quenching law in fact holds over a much broader range of stellar mass (2 dex) and cosmic time. We show that the combination of these two quenching processes, plus some additional quenching due to merging naturally produces (1) a quasi-static single Schechter mass function for star-forming galaxies with an exponential cutoff at a value M* that is set uniquely by the constant of proportionality between the star formation and mass quenching rates and (2) a double Schechter function for passive galaxies with two components. The dominant component (at high masses) is produced by mass quenching and has exactly the same M* as the star-forming galaxies but a faint end slope that differs by Δα\_s \textasciitilde\ 1. The other component is produced by environment effects and has the same M* and α\_s as the star-forming galaxies but an amplitude that is strongly dependent on environment. Subsequent merging of quenched galaxies will modify these predictions somewhat in the denser environments, mildly increasing M* and making α\_s slightly more negative. All of these detailed quantitative inter-relationships between the Schechter parameters of the star-forming and passive galaxies, across a broad range of environments, are indeed seen to high accuracy in the SDSS, lending strong support to our simple empirically based model. We find that the amount of post-quenching "dry merging" that could have occurred is quite constrained. Our model gives a prediction for the mass function of the population of transitory objects that are in the process of being quenched. Our simple empirical laws for the cessation of star formation in galaxies also naturally produce the "anti-hierarchical" run of mean age with mass for passive galaxies, as well as the qualitative variation of formation timescale indicated by the relative α-element abundances.},
    url = "https://doi.org/10.1088/0004-637x/721/1/193",
    doi = "10.1088/0004-637x/721/1/193",
    openalex = "W2074106980",
    references = "doi101046j13658711200306291x, doi101046j13658711200306897x, doi101086154079, doi101086301513, doi101086308692, doi101086376392, doi101088006700491822543, doi101111j13652966200407881x, doi101146annurevastro341749, openalexw3100024326"
}

Many species are experiencing sustained environmental change mainly due to human activities. The unusual rate and extent of anthropogenic alterations of the environment may exceed the capacity of developmental, genetic, and demographic mechanisms that populations have evolved to deal with environmental change. To begin to understand the limits to population persistence, we present a simple evolutionary model for the critical rate of environmental change beyond which a population must decline and go extinct. We use this model to highlight the major determinants of extinction risk in a changing environment, and identify research needs for improved predictions based on projected changes in environmental variables. Two key parameters relating the environment to population biology have not yet received sufficient attention. Phenotypic plasticity, the direct influence of environment on the development of individual phenotypes, is increasingly considered an important component of phenotypic change in the wild and should be incorporated in models of population persistence. Environmental sensitivity of selection, the change in the optimum phenotype with the environment, still crucially needs empirical assessment. We use environmental tolerance curves and other examples of ecological and evolutionary responses to climate change to illustrate how these mechanistic approaches can be developed for predictive purposes.

@article{doi101371journalpbio1000357,
    author = "Chevin, Luis‐Miguel and Lande, Russell and Mace, Georgina M.",
    title = "Adaptation, Plasticity, and Extinction in a Changing Environment: Towards a Predictive Theory",
    year = "2010",
    journal = "PLoS Biology",
    abstract = "Many species are experiencing sustained environmental change mainly due to human activities. The unusual rate and extent of anthropogenic alterations of the environment may exceed the capacity of developmental, genetic, and demographic mechanisms that populations have evolved to deal with environmental change. To begin to understand the limits to population persistence, we present a simple evolutionary model for the critical rate of environmental change beyond which a population must decline and go extinct. We use this model to highlight the major determinants of extinction risk in a changing environment, and identify research needs for improved predictions based on projected changes in environmental variables. Two key parameters relating the environment to population biology have not yet received sufficient attention. Phenotypic plasticity, the direct influence of environment on the development of individual phenotypes, is increasingly considered an important component of phenotypic change in the wild and should be incorporated in models of population persistence. Environmental sensitivity of selection, the change in the optimum phenotype with the environment, still crucially needs empirical assessment. We use environmental tolerance curves and other examples of ecological and evolutionary responses to climate change to illustrate how these mechanistic approaches can be developed for predictive purposes.",
    url = "https://doi.org/10.1371/journal.pbio.1000357",
    doi = "10.1371/journal.pbio.1000357",
    openalex = "W2122485236",
    references = "doi101007bf00344996, doi101007bf00384576, doi101073pnas0709472105, doi101111j13652435200701283x, doi101111j1365294x200703428x, doi101111j14610248200801277x, doi101111j155856461983tb00236x, doi101111j155856461984tb00302x, doi101111j155856461985tb00391x, doi101126science3420403, doi1023072408842, doi105860choice301495"
}