Fermi Degenerate Antineutrino Star Model of Dark Energy

<div>Mass-radius relationship for a neutrino star. The peak occurs at <i>R</i>/<i>a</i> = 1.06 and <i>M</i>/<i>b</i> = 0.356, which for neutrinos of mass <svg height="13.6899pt" id="M26" style="vertical-align:-5.341081pt" version="1.1" viewbox="-0.0498162 -8.34882 48.7037 13.6899" width="48.7037pt" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink"><g transform="matrix(.013,0,0,-0.013,0,0)"><path d="M766 88L752 113C719 83 690 64 681 64C674 64 672 74 679 103L724 292C758 436 724 448 701 448C680 448 666 442 639 429C594 407 514 350 441 252H439L447 289C476 423 450 448 419 448C398 448 379 441 355 427C307 400 234 344 162 249H160L180 324C203 409 197 448 170 448C144 448 82 413 23 349L35 321C57 343 96 374 108 374C115 374 117 371 111 341C87 227 57 112 24 -6L32 -12C53 -4 81 4 108 6C119 68 134 128 149 171C177 229 309 383 364 383C387 383 388 355 373 282C354 190 330 92 303 -6L309 -12C332 -4 356 3 386 6C396 63 411 122 424 171C458 236 590 383 642 383C658 383 664 369 652 315L603 91C587 20 593 -12 619 -12C642 -12 708 23 766 88Z"></path></g><g transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><path d="M213 67C239 136 257 225 255 300C253 353 242 447 164 447C112 447 54 389 41 319L67 309C90 362 117 377 134 377C184 377 189 277 190 239C193 153 164 43 146 -12H176C278 73 450 253 450 390C450 439 410 463 396 463C384 463 380 459 382 449C385 440 389 415 389 402C389 284 312 146 216 67H213Z"></path></g><g transform="matrix(.0065,0,0,-0.0065,14.323,5.233)"><path d="M405 367C405 413 360 454 298 454C251 454 197 434 150 401C64 340 25 235 25 140C25 14 99 -12 150 -12C198 -12 287 5 379 106L360 137C311 89 250 57 202 57C136 57 114 110 114 165V187C210 209 405 256 405 367ZM322 353C322 310 277 263 122 227C137 341 191 386 225 400C233 403 254 409 264 409C299 409 322 394 322 353Z"></path></g><g transform="matrix(.013,0,0,-0.013,21.772,0)"><path d="M535 323V373H52V323H535ZM535 138V188H52V138H535Z"></path></g><g transform="matrix(.013,0,0,-0.013,33.035,0)"><path d="M153 550H386L412 615L406 623H120L82 318C104 327 142 338 184 338C294 338 347 275 347 187C347 112 305 39 221 39C160 39 119 71 97 89C88 97 80 96 71 90C59 80 50 67 49 57C48 45 52 36 66 23C80 9 123 -12 169 -12C221 -11 288 15 342 59C403 109 431 165 431 225C431 308 366 395 238 395C212 395 165 379 127 364L153 550Z"></path></g><g transform="matrix(.013,0,0,-0.013,39.276,0)"><path d="M113 -12C146 -12 170 11 170 46C170 78 146 103 114 103S58 78 58 46C58 11 82 -12 113 -12Z"></path></g><g transform="matrix(.013,0,0,-0.013,42.24,0)"><path d="M241 635C89 635 35 457 35 312C35 153 89 -12 240 -12C390 -12 443 166 443 312C443 466 390 635 241 635ZM238 602C329 602 354 454 354 312C354 172 330 22 240 22C152 22 124 173 124 313S148 602 238 602Z"></path></g></svg> meV/c<sup>2</sup> corresponds to <i>R</i> = 27 billion lightyears (Gly) and <i>M</i> = 1.16 × 10<sup>56</sup> g. At smaller radii, the mass-radius curve corresponds to unstable configurations. Therefore neutrino stars may be relevant for cosmology.</div>

Advances in Astronomy

Fermi Degenerate Antineutrino Star Model of Dark Energy

Figure 1