Cosmologies with Scalar Fields from Higher Dimensions Applied to Bianchi Type <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-4.489pt" id="M1" height="15.5611pt" version="1.1" viewBox="-0.0657574 -11.0721 45.9357 15.5611" width="45.9357pt"><g transform="matrix(.017,0,0,-0.017,0,0)"><path id="g121-84" d="M687 650H462V622C543 612 549 605 530 547C498 447 422 252 372 126H370C302 298 229 492 204 563C188 607 191 615 262 622V650H17V622C77 616 93 608 122 534C180 389 262 172 329 -11H360C436 196 541 450 568 516C606 605 619 614 687 622V650Z"/></g><g transform="matrix(.017,0,0,-0.017,12.063,0)"><path id="g121-71" d="M303 0V28C221 34 213 39 213 125V525C213 610 221 616 303 622V650H38V622C120 616 128 610 128 525V125C128 40 120 34 38 28V0H303Z"/></g><g transform="matrix(.012,0,0,-0.012,17.915,4.134)"><path id="g58-102" d="M522 0V30C462 35 455 41 455 106V280C455 397 397 451 314 451C262 451 206 414 171 379V710C131 698 69 682 20 675V647C87 642 90 637 90 574V106C90 41 80 35 20 30V0H236V30C176 35 171 43 171 106V339C198 371 237 391 276 391C341 391 374 350 374 269V106C374 43 367 35 308 30V0H522Z"/></g><g transform="matrix(.012,0,0,-0.012,24.449,4.134)"><path id="g54-34" d="M556 331V384H55V331H556ZM556 140V193H55V140H556Z"/></g><g transform="matrix(.012,0,0,-0.012,31.788,4.134)"><path id="g54-33" d="M556 236V289H56V236H556Z"/></g><g transform="matrix(.012,0,0,-0.012,39.129,4.134)"><path id="g50-50" d="M389 0V32C297 38 291 46 291 118V635C234 613 175 595 109 583V556L161 554C203 552 207 547 207 497V118C207 46 201 38 110 32V0H389Z"/></g></svg> Model: Classical and Quantum Solutions

<div>Regions where the behaviors of the moduli fields are oscillatory or hyperbolic. The regions outside of the oscillatory and forbidden regions correspond to the hyperbolic behavior.</div>

Advances in High Energy Physics

fig1

Figure 1

Figure 1: Cosmologies with Scalar Fields from Higher Dimensions Applied to Bianchi Type <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-4.489pt" id="M1" height="15.5611pt" version="1.1" viewBox="-0.0657574 -11.0721 45.9357 15.5611" width="45.9357pt"><g transform="matrix(.017,0,0,-0.017,0,0)"><path id="g121-84" d="M687 650H462V622C543 612 549 605 530 547C498 447 422 252 372 126H370C302 298 229 492 204 563C188 607 191 615 262 622V650H17V622C77 616 93 608 122 534C180 389 262 172 329 -11H360C436 196 541 450 568 516C606 605 619 614 687 622V650Z"/></g><g transform="matrix(.017,0,0,-0.017,12.063,0)"><path id="g121-71" d="M303 0V28C221 34 213 39 213 125V525C213 610 221 616 303 622V650H38V622C120 616 128 610 128 525V125C128 40 120 34 38 28V0H303Z"/></g><g transform="matrix(.012,0,0,-0.012,17.915,4.134)"><path id="g58-102" d="M522 0V30C462 35 455 41 455 106V280C455 397 397 451 314 451C262 451 206 414 171 379V710C131 698 69 682 20 675V647C87 642 90 637 90 574V106C90 41 80 35 20 30V0H236V30C176 35 171 43 171 106V339C198 371 237 391 276 391C341 391 374 350 374 269V106C374 43 367 35 308 30V0H522Z"/></g><g transform="matrix(.012,0,0,-0.012,24.449,4.134)"><path id="g54-34" d="M556 331V384H55V331H556ZM556 140V193H55V140H556Z"/></g><g transform="matrix(.012,0,0,-0.012,31.788,4.134)"><path id="g54-33" d="M556 236V289H56V236H556Z"/></g><g transform="matrix(.012,0,0,-0.012,39.129,4.134)"><path id="g50-50" d="M389 0V32C297 38 291 46 291 118V635C234 613 175 595 109 583V556L161 554C203 552 207 547 207 497V118C207 46 201 38 110 32V0H389Z"/></g></svg> Model: Classical and Quantum Solutions 

Advances in High Energy Physics

Cosmologies with Scalar Fields from Higher Dimensions Applied to Bianchi Type Model: Classical and Quantum Solutions

Figure 1