It is in fact astonishing how much deltaV it takes to rendezvous with anything inside Venus' orbit.<br /><br />darkenfast, what you're looking for are the Arjuna class NEOs - but you're not gonna find 'em cuz we can't see 'em.<br /><br />Well actually we have found a few. But it's really tough because they are almost always in the daytime sky and they have a low albedo (they are dark in color). They spot 'em from Mauna Loa at dusk and dawn as we get lucky enough to get a glimpse of objects near their apoapse. IOW, it's no way to make sure we see them all, but it's a start.<br /><br />They're lots and lots and lots of NEOs we can get to easily in terms of dV. The problem is timing. Since the ones that are "close" in terms of orbital radius - so that matching speeds for rendezvous is 'easy' - also have a period close to Earth's, the problem is the timing.<br /><br />It takes a long time for a <i>particular NEO</i> to get lined up for a simple trajectory to it because it goes around the sun at about once per year too. So the 'phase angle' changes slowly. Anyway . . . <br /><br />But there are lots and lots of NEOs to go to, so when you get around to leaving Earth, you can pick out a target at that time. It's just tricky to continue to do business at the same rock.<br /><br />It can be done of course, but essentially you're looking at approx. doubling the trip time from 6 months to 12 months (approx). It's a double Hohmann - you burn for a transfer to an intermediate orbit, coast for six months, and then you burn for the second six-month Hohmann transfer to your rock. (Speaking in very rough terms here)<br /> <div class="Discussion_UserSignature"> </div>