Sounds like she is a piece of trash. Tell everyone you 'did it'. Serve her right. Say she likes anal.

She's not worth you if she's so selfish as to worry about her stupid reputation.

Why did someone post the constitution? WTF! Anyways, that really sucks. That girl is a bitch you deserve better than her.

Definite Bitch. I had the same thing happen with me once.

i say don't even worry about it. i'm sure it sucks right now, but it's better than her trying to completely change everything about you and bothering you to look cool all the time. girls like that try to make everyone act and look exactly how they want them to. i had a friend who did that to me and i was never good enough for her. in a few months you will be happy about this. keep being a great guy, there are girls who will appreciate that. i went for jerks and it did not end well at all, and now i'm with one of the good guys and we are totally happy together. look for the low maintenance girls who just want to spend time with you and do fun shit instead of obsessing about looks and social status.

FederalAgent, you are a good man. Lubby should be jealous.

ROFL

Maybe she has a "social reputation" of sleeping with a different guy every night, and if anyone thought she had a boyfriend, that reputation would be ruined.

Glad for you, OP. You dodged a bullet. It's obvious to me that she is a vain, superficial ****. You probably would've gotten an STD from her, anyways.

well done Federal Agent, why dont i post a bit about my favorite subject in school RG Research: Geodesy Geodesy is the science of measurement of the size, shape, rotation, and gravitational field of the Earth. RG researchers specialize in acquiring, analyzing, interpreting space-based geodetic measurements, and improving the accuracy of such measurements. A variety of processes can influence geodetic measurements over a range of spatial and temporal scales, including: AMP: Atmospheric measurements Studies of the atmospheres of planets in our solar system (including Earth). RG Research: Comets Comets are thought to be among the most primitive bodies left over from the planetesimal building stage of the solar nebula, and so their physical and chemical composition provides an important link between nebular and interstellar processes. A fundamental goal of cometary investigations is to understand the origin and nature of cometary nuclei, in order to explore how they link back to the protoplanetary disk. Of particular interest are parent molecules, those which sublime directly from the nucleus, as measurement of their abundances can reveal relative abundances in the nucleus itself and therefore information about the conditions in which the comet formed. High angular and spectral resolution interferometry is essential to yield constraints on the photochemistry and chemical reactions which occur in the innermost coma since emission on large spatial scales can be selectively resolved out. RG astronomers use the Submillimeter Array to obtain images of thermal dust continuum emission and spectral line emission from the gas molecular species from the inner coma of comets to study the isotopic fractionations and chemical abundances difference between nuclear, extended sources and jets -- gas sublimating from active spots on the nucleus. AMP: X-rays The heliosphere is a bubble of hot gas in interstellar space stretching from the Sun to greater than 100 Sun-Earth distances. It contains some fraction of inflowing neutral interstellar hydrogen and helium atoms. Highly charged positive ions emanate from the Sun in the solar wind and impact the neutral material. The ions capture electrons from the atoms into high excited states that radiate primarily in the soft X-ray spectral region. The spectra provide information about the solar wind composition and velocity and the distribution of atoms in the heliosphere. The X-rays generated by the solar wind contribute to the diffuse soft X-ray background. Similar processes occur in the interaction of the solar wind ions with comets and with the extended exospheres of the planets. We are engaged in theoretical efforts to predict the spectra resulting from the collisions of the solar wind ions (recent references). HEA Research: Planets & Comets Probably the most surprising objects observed in X-rays are comets. Comets were described by Fred Whipple as being "dirty snowballs". So how does a snowball make X-rays? Through a phenomenon called charge exchange. The Sun is constantly streaming ions into the Solar system. Also called the Solar wind, the ions are so highly charged that they will steal electrons from cold gas if possible. A comet becomes active when it gets close to the Sun and it starts putting cold gas out into space. This is when charge exchange can occur. This charge exchange takes place every time an ion gets close to a cold gas molecule, and each time this happens, an X-ray is emitted. This makes comets very bright in X-rays. Comets are so bright that some scientists think we will be able to see comets around other stars in X-rays. Planets have also been detected in X-rays, including the Earth. In addition to charge exchange, which was used to deduce that Mars is losing its atmosphere to space, the most common mechanism is fluorescence. Venus, Jupiter and Saturn have all been detected in X-rays and the physics surrounding the generation of X-rays on each planet has proven to be unique SSP: Solar Physics Our Sun is an excellent laboratory for studying the everyday phenomena of a typical star. SSP scientists are experts in analyzing observations and developing theoretical models of the solar atmosphere, which produces the light we see and where powerful magnetic fields produce hot plasma and accelerate high energy particles that interact with the atmospheres of the Earth and other planets. HEA Research: Sun Introduction: Solar and Stellar X-Ray Group (SSXG) researchers study solar and stellar atmospheres which are composed of extremely hot, highly dynamic plasma. SSXG activities include designing, testing, building and operating instruments, analyzing space and ground-based observations, and creating theoretical models. SSXG researchers are major partners in the Atmospheric Imaging Assembly (AIA) investigation on the Solar Dynamics Observatory, which is set to launch in 2008. SSXG researchers also built the X-Ray Telescope aboard Hinode, which launched in September 2006, the telescope for the Transition Region and Coronal Explorer (TRACE), which launched in 1998, as well as several rockets. HEA Research: Solar Wind X-rays The solar wind originates in the million-degree solar corona and flows out from the sun at a million miles per hour. Most of the ions in the wind are hydrogen and helium, but a small fraction are heavier elements such as carbon, oxygen, and neon. When those heavy ions collide with neutral gas in comets, planetary atmospheres, or very tenuous gas throughout the solar system, they emit X-rays via a process called charge exchange. Many comets and planets have been observed using X-ray telescopes. There is also a diffuse X-ray glow from the Earth's outer atmosphere and from the entire solar system as the solar wind streams out to the edges of the heliosphere, well beyond Pluto. Wherever our X-ray telescopes point, they look through this geocoronal and heliospheric glow. The Local Origin X-rays (LOX) group is a collaboration of CfA and other scientists to observe and model this emission. Charge exchange spectra are also studied in an ongoing laboratory research program. TA: Outer Solar System The CfA has joined the Pan-STARRS-1 Science Consortium. Pan-STARRS-1 is a 1.8m aperture telescope located on Haleakala. Its 1.4 gigapixel, 7 square degree camera will repeatedly image the entire sky north -30 degrees declination. Roughly 60% of the observing time of the PS1 telescope will be dedicated to the "3pi steradian" survey with an observing cadence that is optimized for the detection of near-Earth asteroids and slow-moving solar system bodies. Over the course of its 3.5 year science mission, this unprecedented survey will discover nearly every asteroid, Trojan, Centaur, long-period comet, short-period comet, and trans-neptunian object brighter than magnitude r=23. This census will be used to address a large number of questions regarding the physical and dynamical properties of the various small body populations of the solar system. In addition, this survey will determine the population of large, distant, and rare members of the outer solar system and have the potential to detect planet-sized objects at great distances. The PS1 Outer Solar System key project team is led by Matthew Holman, Associate Director of the Theoretical Astrophysics Division. SSP: Solar System Roughly 4.5 Gyr ago, the Solar System formed in a disk surrounding the proto-Sun. Within this disk, the gas giants grew to their current sizes in a few Myr; the rocky planets took a few tens of Myr to reach their present masses. Besides keeping track of the myriad objects in the Solar System, SSP scientists use data on the compositions, masses, and positions of these objects along with theoretical models to learn how planets form and evolve in time. RG Research: Planets The solar system is comprised of a variety of bodies, from giant planets like Jupiter to the smallest asteroids and everything in between. RG astronomers use the Submillimeter Array to measure both the thermal emission from solar system objects and spectral lines from their atmospheres. These measurements allow one to infer surface temperatures as well as atmospheric composition, thermal structure, and dynamics on bodies as diverse as Neptune, Mars, Titan, and Pluto. SSP: Planet Formation Every planetary system forms in a thin disk of gas and dust orbiting a young star. Small dust grains, a micron or two in size, collide and merge into large aggregates that settle into the midplane of the disk. In the midplane, aggregates grow into planetesimals with diameters of roughly 1 km. Collisions between planetesimals produce planets. SSP scientists use theoretical calculations to understand how dust grains evolve and how planetesimals become planets. SOURCE: All information in this post respectively taken from http://www.cfa.harvard.edu/ssp/star_formation/planetformation.html