Table 2: Scaling output for a planet like $\tau$ Bootes at different stellar system ages (4.6 Gyr, 1.0 Gyr and 0.7 Gyr). See text for details.
$\tau$ Bootes 4.6 Gyr 1.0 Gyr 0.7 Gyr

v(t) (stellar wind velocity) [km s^-1] 400 731 840

n₀(t) (stellar wind density at 1 AU) [m^-3] $1.0\times 10^{7}$ $9.5\times 10^{7}$ $15.9\times 10^{7}$

$\mathcal{M}$ (magnetic moment) [ $\mathcal{M}_{\rm J}$ ] $0.5\ldots2.7$ $0.5\ldots2.7$ $0.5\ldots2.7$

$P_{{\rm rad}}$ (emitted radio power) [W] $0.69\times 10^{14}\ldots2.1\times 10^{14}$ $1.3\times 10^{15}\ldots3.8\times 10^{15}$ $2.5\times 10^{15}\ldots7.3\times 10^{15}$

$\Phi_{{\rm AU}}$ (flux density at 1 AU) [Jy] $4.0\times 10^{10}\ldots9.7\times 10^{10}$ $7.4\times 10^{11}\ldots1.8\times 10^{12}$ $1.4\times 10^{12}\ldots3.5\times 10^{12}$

$\Phi_s$ (flux density at distance s) [Jy] $0.0039\ldots0.0094$ $0.071\ldots0.17$ $0.14\ldots0.33$

$f_{\rm c}^{\max}$ (maximum frequency) [MHz] $6.7\ldots19$ $6.7\ldots19$ $6.7\ldots19$

**Table 2:** Scaling output for a planet like $\tau$ Bootes at different stellar system ages (4.6 Gyr, 1.0 Gyr and 0.7 Gyr). See text for details.
$\tau$ Bootes	4.6 Gyr	1.0 Gyr	0.7 Gyr
v(t) (stellar wind velocity) [km s^-1]	400	731	840
n₀(t) (stellar wind density at 1 AU) [m^-3]	$1.0\times 10^{7}$	$9.5\times 10^{7}$	$15.9\times 10^{7}$
$\mathcal{M}$ (magnetic moment) [ $\mathcal{M}_{\rm J}$ ]	$0.5\ldots2.7$	$0.5\ldots2.7$	$0.5\ldots2.7$
$P_{{\rm rad}}$ (emitted radio power) [W]	$0.69\times 10^{14}\ldots2.1\times 10^{14}$	$1.3\times 10^{15}\ldots3.8\times 10^{15}$	$2.5\times 10^{15}\ldots7.3\times 10^{15}$
$\Phi_{{\rm AU}}$ (flux density at 1 AU) [Jy]	$4.0\times 10^{10}\ldots9.7\times 10^{10}$	$7.4\times 10^{11}\ldots1.8\times 10^{12}$	$1.4\times 10^{12}\ldots3.5\times 10^{12}$
$\Phi_s$ (flux density at distance s) [Jy]	$0.0039\ldots0.0094$	$0.071\ldots0.17$	$0.14\ldots0.33$
$f_{\rm c}^{\max}$ (maximum frequency) [MHz]	$6.7\ldots19$	$6.7\ldots19$	$6.7\ldots19$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Stellar radio flux
	3 Planetary radio flux
	4 Radio emission and stellar system age
	5 Radio comparison
	6 Conclusion
	References