Difference between revisions of "Variable Stars"
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| − | + | =Classification= | |
Variable stars may be either ''intrinsic'' or ''extrinsic''. | Variable stars may be either ''intrinsic'' or ''extrinsic''. | ||
| + | ==Intrinsic Variable Stars== | ||
*'''Intrinsic variable stars''': stars where the variability is being caused by changes in the physical properties of the stars themselves. This category can be divided into three subgroups. | *'''Intrinsic variable stars''': stars where the variability is being caused by changes in the physical properties of the stars themselves. This category can be divided into three subgroups. | ||
| − | |||
**Eruptive variables, stars who experience eruptions on their surfaces like flares or mass ejections. | **Eruptive variables, stars who experience eruptions on their surfaces like flares or mass ejections. | ||
| − | **Cataclysmic or explosive variables, stars that undergo a cataclysmic change in their properties like [[nova]]e and [[supernova]]e. | + | **Pulsating variables, stars whose radius alternately expands and contracts as part of their natural evolutionary ageing processes. |
| + | **Cataclysmic or explosive variables, stars that undergo a cataclysmic change in their properties like [[nova]]e and [[supernova]]e. Interacting binary systems with white dwarfs or stars showing large amplitude outbursts. | ||
| + | 1. Eruptive | ||
| + | FU, GCAS, I, IA, IB, IN, INA, INB, INT, IT, IN(YY), IS, ISA, ISB, RCB, RS, SDOR, UV, UVN, WR | ||
| + | 2. Pulsating | ||
| + | ACYG, BCEP, BCEPS, CEP, CEP(B), CW, CWA, CWB, DCEP, DCEPS, DSCT, DSCTC, GDOR, L, LB, LC, M, PVTEL, RPHS, RR, RR(B), RRAB, RRC, RV, RVA, RVB, SR, SRA, SRB, SRC, SRD, SXPHE, ZZ, ZZA, ZZB | ||
| + | 3. Cataclysmic (explosive and novalike) variables | ||
| + | N, NA, NB, NC, NL, NR, SN, SNI, SNII, UG, UGSS, UGSU, UGZ, ZAND | ||
| + | |||
| + | |||
| + | ==Extrinsic Variable Stars== | ||
*'''Extrinsic variable stars''': stars where the variability is caused by external properties like rotation or eclipses. There are two main subgroups. | *'''Extrinsic variable stars''': stars where the variability is caused by external properties like rotation or eclipses. There are two main subgroups. | ||
| − | **Eclipsing binaries, | + | **Eclipsing binaries, double stars where, as seen from Earth's vantage point the stars occasionally eclipse one another as they orbit. |
| + | |||
| + | 4. Eclipsing binary systems | ||
| + | E, EA, EB, EW, GS, PN, RS, WD, WR, AR, D, DM, DS, DW, K, KE, KW, SD | ||
| + | |||
**Rotating variables, stars whose variability is caused by phenomena related to their rotation. Examples are stars with extreme "sunspots" which affect the apparent brightness or stars that have fast rotation speeds causing them to become ellipsoidal in shape. | **Rotating variables, stars whose variability is caused by phenomena related to their rotation. Examples are stars with extreme "sunspots" which affect the apparent brightness or stars that have fast rotation speeds causing them to become ellipsoidal in shape. | ||
| − | + | 5. Rotating | |
| + | ACV, ACVO, BY, ELL, FKCOM, PSR, SXARI | ||
| − | |||
| − | + | ||
| + | 6. intense variable X-ray sources (X, XB, XF, XI, XJ, XND, XNG, XP, XPR, | ||
| + | XPRM, XM), | ||
| + | 7. other symbols (BLLAC, CST, GAL, L:, QSO, S, *, +, :). | ||
| + | 8. the new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB) | ||
Latest revision as of 21:02, 18 May 2014
A variable star is a star where its brightness as seen from Earth fluctuates. The study of variable stars involves the recording of its magnitude, and how that fluctuates over time. The plotting of a variable star's magnitude vs. time is known as a light curve. The light curve plotting of variable stars combined with the study of supernovae events help physicists understand the formation of the universe.
Classification
Variable stars may be either intrinsic or extrinsic.
Intrinsic Variable Stars
- Intrinsic variable stars: stars where the variability is being caused by changes in the physical properties of the stars themselves. This category can be divided into three subgroups.
- Eruptive variables, stars who experience eruptions on their surfaces like flares or mass ejections.
- Pulsating variables, stars whose radius alternately expands and contracts as part of their natural evolutionary ageing processes.
- Cataclysmic or explosive variables, stars that undergo a cataclysmic change in their properties like novae and supernovae. Interacting binary systems with white dwarfs or stars showing large amplitude outbursts.
1. Eruptive
FU, GCAS, I, IA, IB, IN, INA, INB, INT, IT, IN(YY), IS, ISA, ISB, RCB, RS, SDOR, UV, UVN, WR
2. Pulsating
ACYG, BCEP, BCEPS, CEP, CEP(B), CW, CWA, CWB, DCEP, DCEPS, DSCT, DSCTC, GDOR, L, LB, LC, M, PVTEL, RPHS, RR, RR(B), RRAB, RRC, RV, RVA, RVB, SR, SRA, SRB, SRC, SRD, SXPHE, ZZ, ZZA, ZZB
3. Cataclysmic (explosive and novalike) variables
N, NA, NB, NC, NL, NR, SN, SNI, SNII, UG, UGSS, UGSU, UGZ, ZAND
Extrinsic Variable Stars
- Extrinsic variable stars: stars where the variability is caused by external properties like rotation or eclipses. There are two main subgroups.
- Eclipsing binaries, double stars where, as seen from Earth's vantage point the stars occasionally eclipse one another as they orbit.
4. Eclipsing binary systems
E, EA, EB, EW, GS, PN, RS, WD, WR, AR, D, DM, DS, DW, K, KE, KW, SD
- Rotating variables, stars whose variability is caused by phenomena related to their rotation. Examples are stars with extreme "sunspots" which affect the apparent brightness or stars that have fast rotation speeds causing them to become ellipsoidal in shape.
5. Rotating
ACV, ACVO, BY, ELL, FKCOM, PSR, SXARI
6. intense variable X-ray sources (X, XB, XF, XI, XJ, XND, XNG, XP, XPR,
XPRM, XM),
7. other symbols (BLLAC, CST, GAL, L:, QSO, S, *, +, :). 8. the new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB)
