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  2. Phase transition - Wikipedia

    en.wikipedia.org/wiki/Phase_transition

    In physics, chemistry, and other related fields like biology, a phase transition (or phase change) is the physical process of transition between one state of a medium and another. Commonly the term is used to refer to changes among the basic states of matter : solid , liquid , and gas , and in rare cases, plasma .

  3. Scale factor (cosmology) - Wikipedia

    en.wikipedia.org/wiki/Scale_factor_(cosmology)

    In physical cosmology, the dark-energy-dominated era is proposed as the last of the three phases of the known universe, the other two being the radiation-dominated era and the matter-dominated era. The dark-energy-dominated era began after the matter-dominated era, i.e. when the Universe was about 9.8 billion years old. [13]

  4. List of states of matter - Wikipedia

    en.wikipedia.org/wiki/List_of_states_of_matter

    Time crystals: A state of matter where an object can have movement even at its lowest energy state. Hidden states of matter: Phases that are unattainable or do not exist in thermal equilibrium, but can be induced e.g. by photoexcitation. Microphase separation: Constituent units forming diverse phases while also keeping united.

  5. Intensive and extensive properties - Wikipedia

    en.wikipedia.org/wiki/Intensive_and_extensive...

    An extensive property is a physical quantity whose value is proportional to the size of the system it describes, [8] or to the quantity of matter in the system. For example, the mass of a sample is an extensive quantity; it depends on the amount of substance.

  6. Physical change - Wikipedia

    en.wikipedia.org/wiki/Physical_change

    A physical change involves a change in physical properties. Examples of physical properties include melting, transition to a gas, change of strength, change of durability, changes to crystal form, textural change, shape, size, color, volume and density. An example of a physical change is the process of tempering steel to

  7. Steady-state model - Wikipedia

    en.wikipedia.org/wiki/Steady-state_model

    On the other hand, the steady-state model says while the universe is expanding, it nevertheless does not change its appearance over time (the perfect cosmological principle). E.g., the universe has no beginning and no end. This required that matter be continually created in order to keep the universe's density from decreasing.

  8. Friedmann equations - Wikipedia

    en.wikipedia.org/wiki/Friedmann_equations

    The Hubble parameter can change over time if other parts of the equation are time dependent (in particular the mass density, the vacuum energy, or the spatial curvature). Evaluating the Hubble parameter at the present time yields Hubble's constant which is the proportionality constant of Hubble's law.

  9. Changes in matter - Wikipedia

    en.wikipedia.org/wiki/Changes_in_matter

    Download as PDF; Printable version; ... Changes in matter may refer to: Chemical changes in matter; Physical changes in matter This page was last edited on 28 ...