Dynamic dilution equation for stars¶
Summary¶
Fit DTD Theory for stars. Theory of stress relaxation in star polymer melts with no adjustable parameters beyond those measurable in linear melts
- Function
See Milner-McLeish (1997) and Larson et al. (2003) for details.
- Parameters
G0
\(\equiv G_N^0\): Plateau modulustau_e
\(\equiv \tau_\mathrm e = \left(\dfrac{M_\mathrm e^\mathrm G}{M_0}\right)^2 \dfrac{\zeta b^2}{3\pi^2k_\mathrm B T}\): Entanglement equilibration timeMe
\(\equiv M_\mathrm e^\mathrm G = \dfrac 4 5 \dfrac{\rho R T} {G_N^0}\): Entanglement molecular weightalpha
: Dilution exponent
- where:
\(\rho\): polymer density
\(\zeta\): monomeric friction coefficient
\(b\): monomer-based segment length
\(k_\mathrm B T\): thermal energy
\(M_0\): molar mass of an elementary segment