Changes

VV Cephei A is thought to have a [[mass (science)|mass]] of 20 [[solar mass]]es and a radius approximately 1,000 times that of the [[Sun]], though more older measurements place it higher at 1,600 times the solar radius.<ref name=variablePaper/><ref name=contellationguide>{{cite web|url=https://www.constellation-guide.com/constellation-list/cepheus-constellation/|title=Cepheus Constellation|accessdate=January 30, 2020|publisher=constellation-guide}}</ref> For a comparison, if it were to replace the Sun in our [[solar system]], its surface would easily extend to the orbit of [[Saturn]] or possibly [[Uranus]].<ref>{{cite web|url=https://thesciencearchives.miraheze.org/wiki/VV_Cephei|title=VV Cephei|accessdate=January 30, 2020|publisher=thesciencearchives.miraheze.org|date=November 24, 2018}}</ref> The temeprature of its surface it thought to be in the range 3,300-3,650&nbsp;kelvin and its [[luminosity]] is estimated to be 400,000 larger than the Sun's.<ref name=illinois/> The star is a pulsating semi-regular variable star and changes in brightness by several hundredths to a few tenths of magnitude as it pulsates. These changes take place over several times periods 58, 118, and 349 days as well as an additional one of 13.7 years. VV Cephei A's shape is not thought to be spherical, but something closer to a teardrop shape, though more subtle. The star is sufficiently larger that there is a [[Doppler-shift]] in the [[hydrogen]]-alpha line in the star's spectrum. This is causes by the star's rotation as one side of the star is rotating towards us and so light from that side is [[blueshift|blue shifted]] whereas light from the side rotating away from us is [[redshift|red shifted]].<ref name=variablePaper/>

VV Cephei A is thought to have a [[mass (science)|mass]] of 20 [[solar mass]]es and a radius approximately 1,000 times that of the [[Sun]], though more older measurements place it higher at 1,600 times the solar radius.<ref name=variablePaper/><ref name=contellationguide>{{cite web|url=https://www.constellation-guide.com/constellation-list/cepheus-constellation/|title=Cepheus Constellation|accessdate=January 30, 2020|publisher=constellation-guide}}</ref> For a comparison, if it were to replace the Sun in our [[solar system]], its surface would easily extend to the orbit of [[Saturn]] or possibly [[Uranus]].<ref>{{cite web|url=https://thesciencearchives.miraheze.org/wiki/VV_Cephei|title=VV Cephei|accessdate=January 30, 2020|publisher=thesciencearchives.miraheze.org|date=November 24, 2018}}</ref> The temeprature of its surface it thought to be in the range 3,300-3,650&nbsp;kelvin and its [[luminosity]] is estimated to be 400,000 larger than the Sun's.<ref name=illinois/> The star is a pulsating semi-regular variable star and changes in brightness by several hundredths to a few tenths of magnitude as it pulsates. These changes take place over several times periods 58, 118, and 349 days as well as an additional one of 13.7 years. VV Cephei A's shape is not thought to be spherical, but something closer to a teardrop shape, though more subtle. The star is sufficiently larger that there is a [[Doppler-shift]] in the [[hydrogen]]-alpha line in the star's spectrum. This is causes by the star's rotation as one side of the star is rotating towards us and so light from that side is [[blueshift|blue shifted]] whereas light from the side rotating away from us is [[redshift|red shifted]].<ref name=variablePaper/>

Although smaller than VV Cephei A, VV Cephei B is still quite large compared to the Sun with an estimated mass in the neighbourhood of 19 solar masses and radius of 13 solar radii.<ref>{{cite journal

Although smaller than VV Cephei A, VV Cephei B is still quite large compared to the Sun with an estimated mass in the neighbourhood of 19 solar masses and radius of 13 solar radii.<ref name=variablePaper/><ref>{{cite journal

  |last1=Hutchings |first1=J. B.

  |last1=Hutchings |first1=J. B.

  |last2=Wright |first2=K. O.

  |last2=Wright |first2=K. O.

  |bibcode=1971MNRAS.155..203H

  |bibcode=1971MNRAS.155..203H

  |ref=harv

  |ref=harv

}}</ref><ref name=variablePaper/> The star dominates the spectrum of the VV Cephei system in the [[ultraviolet]] and at higher wavelengths whereas VV Cephei A dominated in the [[infrared]]. The star appears blue-white in color and its class is a B6 dwarf.<ref name=illinois/>

}}</ref> The star dominates the spectrum of the VV Cephei system in the [[ultraviolet]] and at higher wavelengths whereas VV Cephei A dominated in the [[infrared]]. The star appears blue-white in color and its class is a B6 dwarf.<ref name=illinois/>

==References==

==References==