Binding Site Structure and Stoichiometry in Serotonin Type 3 Receptors

This dissertation primarily describes studies of serotonin type 3 (5-HT₃) receptors of the Cys-loop super-family of ligand gated ion channels. The first chapter provides a general introduction to these important proteins and the methods used to interrogate their structure and function. The second chapter details the delineation of a structural unit of the ligand binding site of homomeric 5-HT₃A receptors on which the ligands serotonin (5-HT) and m-chlorophenyl biguanide (mCPBG) are reliant for effective receptor activation. Unnatural amino acid mutagenesis results show that the details of each ligand’s interaction with this organizing feature of the binding site differ, providing insights into general principles of receptor activation.

The third chapter describes a study in which florescent protein fusions of the A and B subunits of the heteromeric 5-HT₃AB receptor are employed to determine the subunit stoichiometry and order within functional receptors. Strong evidence is found for an A₃B₂ stoichiometry with A-A-B-A-B order. The fourth chapter investigates the potential for ligand binding across heteromeric binding sites in the 5-HT₃AB receptor. Unlike serotonin, mCPBG is found to bind the receptor at heteromeric binding sites. Further mCPBG is capable of allosterically modulating the response of serotonin on the 5-HT₃AB receptor from these heteromeric sites.

Finally, the fifth chapter describes progress towards the application of unnatural amino acid mutagenesis to an important new class of proteins, transcription factors. Experiments optimizing novel methods for the detection of function are described, using RARα of the nuclear receptor family of transcription factors.

The streaming of 1.3-2.3 MeV cosmic-ray protons during periods between prompt solar particle events

The anisotropy of 1.3 - 2.3 MeV protons in interplanetary space has been measured using the Caltech Electron/Isotope Spectrometer aboard IMP-7 for 317 6-hour periods from 72/273 to 74/2. Periods dominated by prompt solar particle events are not included. The convective and diffusive anisotropies are determined from the observed anisotropy using concurrent solar wind speed measurements and observed energy spectra. The diffusive flow of particles is found to be typically toward the sun, indicating a positive radial gradient in the particle density. This anisotropy is inconsistent with previously proposed sources of low-energy proton increases seen at 1 AU which involve continual solar acceleration.

The typical properties of this new component of low-energy cosmic rays have been determine d for this period which is near solar minimum. The particles have a median intensity of 0.06 protons/ cm^(2)-sec-sr-MeV and a mean spectral index of -3.15.The amplitude of the diffusive anisotropy is approximately proportional to the solar wind speed. The rate at which particles are diffusing toward the sun is larger than the rate at which the solar wind is convecting the particles away from the sun. The 20 to 1 proton to alpha ratio typical of this new component has been reported by Mewaldt, et al. (1975b).

A propagation model with κ_(rr) assumed independent of radius and energy is used to show that the anisotropy could be due to increases similar to those found by McDonald, et al. (1975) at ~3 AU. The interplanetary Fermi-acceleration model proposed by Fisk (1976) to explain the increases seen near 3 AU is not consistent with the ~12 per cent diffusive anisotropy found.

The dependence of the diffusive anisotropy on various parameters is shown. A strong dependence of the direction of the diffusive anisotropy on the concurrently measured magnetic field direction is found, indicating a κ_⊥ less than κ_∥ to be typical for this large data set.