Kdot hit the orbital mechanics question, though I suspect it's even a bit more interesting than that. (Ooh! It is! Look up Lissajous Orbit and Halo Orbit on Wikipedia. If you can use an orbit around a Lagrange point, they might work for you. Oh,yes: Look up Lagrangian Point, too.) But first I'd like to talk about your planet's thermal equilibrium. I'm going to belabor some basic points so you can follow the question a bit more deeply.
Heat is transferred though 'empty' space by radiation--light, that is, and mostly infrared for a habitable planet. When we on the surface face the sun (daytime) we soak up its heat. When we face the deep dark of space (nighttime) we radiate heat out into that abysssal void. The very delicate balance of heat absorbed and heat released creates the narrow band of temperature in which life is possible on most of our planet. And they most important limits are the melting/freezing point of water and the temperatures at which proteins start to denature. (Forget about silicon-based life. Bonds between silicon atoms are too damn strong. No adhesive will bond to silicone. Not even silicone adhesive.)
The next thing to understand is the inverse-square law. This follows from a simple geometric reality: The surface area of sphere increases in proportion to the square of the sphere's radius. If an energy source (like a sun) is radiating in all directions from the center of a hollow sphere, the total energy released to the sphere is the same no matter the size of the sphere. But the energy that hits a patch of fixed area is a fraction of the total, and the fraction is the fixed area divided by the surface area of the sphere. Since that area goes as the square of the sphere's radius, the energy available to that patch of fixed area goes as the inverse of the square of the radius. And since the intensity of the energy flow (ie., the 'flux') is measured as energy per unit area, the intensity of radiation from your sun falls off as the square of the distance from the sun.
A nearly circular orbit will provide a nearly constant luminous intensity to the planet. A highly elliptical orbit--or a figure-eight orbit--will create immense swings in heating and cooling. Moreover, the planet's velocity will be highest at its nearest approach to the sun, where its gravitational potential energy is the lowest. The sum of potential energy and kinetic energy of motion will be constant (neglecting relativistic and tidal losses over cosmic ages). Note also that kinetic energy goes as the square of the speed. In a noticeably elliptical orbit, your planet will race through a hot zone in one short season and mosey languidly through the heat-absorbing blackness of the void for the opposite, much longer season. Life as we know it on earth is possible because earth's orbit is very nearly circular.
(A digression on ellipses: In an elliptical orbit, a light body travels in an ellipse around a much heavier body--and this isn't quite right; see below--with the heavy body at one of the two focus points of the ellipse. The focus points lie on the major axis of the ellipse, and every point on the ellipse meets two constraints. First, all points are in one plane. Second, for each point the sum of the distances from the point to the two fociii is constant.)
Next question: When is a square foot not a square foot? (If you are too square for feet, substitute 'meter'. It's just a constant factor.) Well ...
Imagine you are standing on earth, on a sunny day. You hold in your hands a sheet of material one foot square, and you hold that sheet perpendicular to the sun's rays. It receives one square foot of solar radiation.
Then you turn that sheet about an axis in the plane of the sheet, so that the plane of the sheet is no longer perpendicular to the sun's rays, but instead lies at an angle of 30 degrees from them. Along the axis on which you rotated the sheet, the sheet still shadows the same distance it shadowed before, but along an axis perpendicular to the rotation axis (and perpendicular to the sun's rays) the shadow is shortened by half. Your square foot of sheet is absorbing only half a square foot's worth of solar radiation because it is canted to 'look llike' half a square foot 'to the sun'.
You may be noticing a theme here Geometry Rules! As always and ever it has.
Imagine now that you are standing on the earth's equator at high noon (local high noon) at one of the equinoxes. You hold your foot-square sheet parallel to the surface of the earth (ie., perpendicular to a plumb line). It receives one square foot worth of solar radiation. (We'll neglect losses to the atmosphere to keep the problem simple.) Imagine next that you are standing in Cairo, at local high noon, on the equinox. Cairo is at thirty degrees north latitude, so your plumb line lies thirty degrees away from the line of solar radiation. Your foot-square sheet now looks like root-three-over-two feet (about 0.87 square feet) to the sun.
Move to Montreal, at 45 degrees north latitude, local high noon on the equinox. Your 'horizontal' square foot sheet presents only root-two-over-two square feet to the sun. And when you set your square foot up in Helsinki at local high noon on the equinox at sixty degrees north latitude, you'll be presenting only half a square foot to the ever-generous sun and its radiation.
Belabor, belabor, belabor ...
Okay, we're getting to seasons and tilt of the planet's rotational axis. I'm assuming that your planet will have at least some of that. You could make it weird and have the axis in the plane of the orbit, but that means that during the 'year' there will be times when one hemisphere is in continual hot day and the other is in frigid, sky-void-cold night. (Speaking of planetary rotation, will your planet have a magnetic field? Very good for keeping particle radiation away from the surface.)
You're going to have to figure out how much energy is coming off each sun, and how that relates to stellar mass and age. (See Stellar Evolution on Wikipedia.) Small, even very small, changes will have major consequences over time.
Remember when you learned that the earth orbits the sun? Well, that's a lie. The earth orbits the center of mass of the solar system, and because Jupiter is so massive, it pulls that center of mass outside the sun's corona. The other planets can increase or decrease this effect, depending on where they are relative to Jupiter. This means that earth is sometimes closer to the sun than at other times, depending on the position of Jupiter, and that is one reason why we have long-term cycles in climate. (Solar sunspot cycles are another reason.)