D T IN ENGLISH TRANSLATION

• d t

Examples of using D t in Spanish and their translations into English

la correspondiente ecuación dada por el teorema de Ehrenfest toma la forma: d d t⟨ A⟩ i ℏ⟨⟩{\displaystyle{\frac{d}{dt}}\langleA\rangle={\frac{i}{\hbar}}\langle\rangle}
the corresponding equation is given by Ehrenfest's theorem, and takes the form d d t⟨ A⟩ 1 i ℏ⟨⟩{\displaystyle{\frac{d}{dt}}\langle A\rangle={\frac{1}{i\hbar}}\langle\rangle}

0 S d T- V d p+∑ i N i d μ i{\displaystyle 0=SdT-Vdp+\sum_{ i}
0 S d T- V d p+∑ i N i d μ i{\displaystyle 0=SdT-Vdp+\sum_{ i}

n- 1 f( t) d t,{\displaystyle( J^{ n}
n- 1 f( t) d t,{\displaystyle( J^{ n}

la métrica de Peres se define por el tiempo propio d τ 2 d t 2- 2 f( t+ z, x, y)( d t+ d z)
the Peres metric is defined by the proper time d τ 2 d t 2- 2 f( t+ z, x, y)( d t+ d z)

V L L d I d t{\displaystyle V_{L}=L{\frac{dI}{dt}}}
V L L d I d t{\displaystyle V_{L}=L{\frac{dI}{dt}}}

γ′( t)| d t{\displaystyle L=\int_{ a}^{ b}|\ gamma'(t)|\,
γ′( t)| d t{\displaystyle L=\int_{ a}^{ b}|\ gamma'(t)|\,

Esta ecuación puede ser resuelta exactamente; la solución es simplemente la integral de pp. Esto sugiere que: y n+ s y n+ s- 1+∫ t n+ s- 1 t n+ s p( t) d t.{\displaystyle y_{ n+s}= y_{ n+s-1}+\ int_{ t_{ n+s-1}}^{ t_{ n+s}}
This suggests taking y n+ s y n+ s- 1+∫ t n+ s- 1 t n+ s p( t) d t.{\displaystyle y_{ n+s}= y_{ n+s-1}+\ int_{ t_{ n+s-1}}^{ t_{ n+s}}

d 2 x d t 2- μ( 1- x 2) d x d t+ x 0{\displaystyle{d^{2}x\over dt^{2}}-\mu(1-x^{2}){dx\over dt}+x=0}
d 2 x d t 2- μ( 1- x 2) d x d t+ x 0,{\displaystyle{d^{2}x\over dt^{2}}-\mu(1-x^{2}){dx\over dt}+x=0,}

d P d t r P( 1- P K){\displaystyle{\frac{ dP}{ dt}}= rP\ left( 1-{\ frac{ P}{ K}}\ right)}
d P d t r P⋅( 1- P K){\displaystyle{\frac{ dP}{ dt}}= rP\ cdot\left(1-{\frac{ P}{ K}}\ right)} where the constant

se da de la siguiente forma: η∫ 0 t d t′ a( t′){\displaystyle\eta=\int_{ 0}^{ t}{\ frac{ dt'}{ a( t')}}}
certain time t{\displaystyle t} is given by η∫ 0 t d t′ a( t′),{\displaystyle\eta=\int_{ 0}^{ t}{\ frac{dt'}{at where a( t){\displaystyle a(t)}

Entonces, el derivado material del escalar φ es D φ D t∂ φ∂ t+ u⋅∇ φ.{\displaystyle{\frac{\mathrm{D}\varphi}{\mathrm{D} t}}={\frac{\partial\varphi}{\partial t}}+\mathbf{u}\cdot\nabla\ varphi.}
So, the material derivative of the scalar φ is D φ D t∂ φ∂ t+ u⋅∇ φ.{\displaystyle{\frac{\mathrm{D}\varphi}{\mathrm{D} t}}={\frac{\partial\varphi}{\partial t}}+\mathbf{u}\cdot\nabla\ varphi.}

Si en la relación d P(∂ P∂ S) T d S+(∂ P∂ T) S d T{\displaystyle dP=\left({\frac{\partial P}{\partial S}}\ right)_{ T} dS+\ left({\ frac{\partial P}{\partial T}}\ right)_{ S} dT\,} Se puede sustituir d P 0{\displaystyle dP=0} y resolver la relación d S d T{\displaystyle{\frac{dS}{dT}}} obtendremos(∂ S∂ T)
If in the relation d P(∂ P∂ S) T d S+(∂ P∂ T) S d T{\displaystyle dP=\left({\frac{\partial P}{\partial S}}\ right)_{ T} dS+\ left({\ frac{\partial P}{\partial T}}\ right)_{ S} dT\,} we put d P 0{\displaystyle dP=0} and solve for the ratio d S d T{\displaystyle{\frac{dS}{dT}}} we obtain(∂ S∂ T)

1. d N i d t F i o- F i+ V v i r i{\displaystyle{dNi\over dt}=Fio-Fi+Vviri} Dónde Fio es la entrada de velocidad de flujo molar de especies i,
1. d N i d t F i o- F i+ V ν i r i{\displaystyle{\frac{ dN_{ i}}{ dt}}= F_{ io}- F_{ i}+ V\ nu_{i}r_{i}}

θ t d t+ σ d W t{\displaystyle d\ln(r)=\theta_{t}\,
θ t d t+ σ d W t{\displaystyle d\ln(r)=\theta_{t}\,

d x d t K( t c- t)
d x d t K( t c- t)

conjeturó que el número de primos menores o iguales que un número N grande es muy próximo al valor de la siguiente integral∫ 2 N 1 log⁡( t) d t.{\displaystyle\,\int_{ 2}^{ N}{\ frac{ 1}{\ log( t)}}\,
conjectured that the number of primes less than or equal to a large number N is close to the value of the integral∫ 2 N 1 log t d t.{\displaystyle\,\int_{ 2}^{ N}{\ frac{1}{\log\, t}}\, dt.}

T g→ T 0 c as d T d t→ 0.{\displaystyle T_{g}\to T_{0c}{\text{ as}}{\frac{dT}{dt}}\to 0.} El modelo de Gibbs-DiMarzio predice específicamente que la entropía
T g→ T 0 c as d T d t→ 0.{\ displaystyle T_{ g}\ to T_{ 0c}{\ text{ as}}{\ frac{ dT}{ dt}}\ to 0.}

Descubierto por Karl Schwarzschild, el criterio de Schwarzschild es un criterio en astrofísica donde un medio estelar es estable contra la convección donde- d T d Z< g C p{\displaystyle-{\frac{dT}{dZ}}.
Discovered by Karl Schwarzschild, the Schwarzschild criterion is a criterion in astrophysics where a stellar medium is stable against convection where- d T d Z< g C p{\displaystyle-{\frac{dT}{dZ}}.

El cociente de ambos coeficientes: S T D T D{\displaystyle S_{T}={\frac{ D_{ T}}{ D}}} se llama coeficiente de Soret.
The quotient of both coefficients S T D T D{\displaystyle S_{T}={\frac{ D_{ T}}{ D}}} is called Soret coefficient.

E y/ B z d T/ d x,{\displaystyle|N|={\frac{ E_{ y}/ B_{ z}}{ dT/ dx}},}
E Y/ B Z d T/ d x{\displaystyle|N|={\frac{ E_{ Y}/ B_{ Z}}{ dT/ dx}}}