radio star Comparison Table

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radio star comparison table

Subject has spectral type is part of has acceptance statu has frequency has optical brightness variation has observational problem has light curve has symbol has acronym has abundance has recovery time has amplitude has charge has outburst start time has wavelength is a kind of has peak brightness has name designated with has observable variation time scale has synonym has definition has luminosity class obey

flare star M 0.2 magnitudes or greater some difficulty in distinguishing between various kinds d CV 70 percent of all stars red dwarf
R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name
RR, RS, RT, RU, RV, RW, RX, RY, or RZ and the genitive of the latin constellation name when the single letter designations are exhausted
AA...AZ, BB...BZ, etc. (omitting J), which ends with QQ...QZ and the genitive of the latin constellation namewhen the RR...RZ designations are exhausted
V 335, V 336, etc., when the double letter designations are exhausted
within a period of decades UV Ceti star Stars undergoing erratic jumps in brightness (up to a few magnitudes) on time scales of the order of minutes. During the quiescent phase the spectrum is that of an M dwarf with emissions in the CaII and Balmer lines. V

pulsar dark halo hypothetical inversely proportional to the wavelength PSR inversely proportional to its momentum radio star hidden mass An object discovered at Cambridge University in 1967 which has the mass of a star and a radius no larger than that of Earth and which emits radio pulses with a very high degree of regularity (periods range from 0.03 s for the youngest to more than 3 s for the oldest). All pulsars are characterized by the general properties of dispersion, periodicity, and short duty cycle. Pulsars are believed to be rotating, magnetic (surface magnetic fields of 10¹⁰ to 10¹⁴ gauss are estimated) neutron stars which are the end products of supernovae. Type S pulsars have a simple pulse shape: Type C, complex: Type D have drifting subpulses. uncertainty principle

Next star: spectrum variable Up: star Previous star: program star

Subject	has spectral type	is part of	has acceptance statu	has frequency	has optical brightness variation	has observational problem	has light curve	has symbol	has acronym	has abundance	has recovery time	has amplitude	has charge	has outburst start time	has wavelength	is a kind of	has peak brightness	has name designated with	has observable variation time scale	has synonym	has definition	has luminosity class	obey
flare star	M				0.2 magnitudes or greater	some difficulty in distinguishing between various kinds		d	CV	70 percent of all stars						red dwarf		R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name RR, RS, RT, RU, RV, RW, RX, RY, or RZ and the genitive of the latin constellation name when the single letter designations are exhausted AA...AZ, BB...BZ, etc. (omitting J), which ends with QQ...QZ and the genitive of the latin constellation namewhen the RR...RZ designations are exhausted V 335, V 336, etc., when the double letter designations are exhausted	within a period of decades	UV Ceti star	Stars undergoing erratic jumps in brightness (up to a few magnitudes) on time scales of the order of minutes. During the quiescent phase the spectrum is that of an M dwarf with emissions in the CaII and Balmer lines.	V
pulsar		dark halo	hypothetical	inversely proportional to the wavelength					PSR						inversely proportional to its momentum	radio star				hidden mass	An object discovered at Cambridge University in 1967 which has the mass of a star and a radius no larger than that of Earth and which emits radio pulses with a very high degree of regularity (periods range from 0.03 s for the youngest to more than 3 s for the oldest). All pulsars are characterized by the general properties of dispersion, periodicity, and short duty cycle. Pulsars are believed to be rotating, magnetic (surface magnetic fields of 10¹⁰ to 10¹⁴ gauss are estimated) neutron stars which are the end products of supernovae. Type S pulsars have a simple pulse shape: Type C, complex: Type D have drifting subpulses.		uncertainty principle