66 results on '"Klimchuk, J. A."'
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2. Transition Region Contribution to AIA Observations in the Context of Coronal Heating
3. Erratum: “The Role of Magnetic Helicity in Coronal Heating” (2019, ApJ, 883, 26)
4. Spectroscopic Constraints on the Cross-sectional Asymmetry and Expansion of Active Region Loops
5. The Role of Magnetic Helicity in Coronal Heating
6. Power-law Statistics of Driven Reconnection in the Magnetically Closed Corona
7. UNRAVELLING THE COMPONENTS OF A MULTI-THERMAL CORONAL LOOP USING MAGNETOHYDRODYNAMIC SEISMOLOGY
8. HOW GAS-DYNAMIC FLARE MODELS POWERED BY PETSCHEK RECONNECTION DIFFER FROM THOSE WITH AD HOC ENERGY SOURCES
9. CHROMOSPHERIC NANOFLARES AS A SOURCE OF CORONAL PLASMA. II. REPEATING NANOFLARES
10. ARE CHROMOSPHERIC NANOFLARES A PRIMARY SOURCE OF CORONAL PLASMA?
11. CORE AND WING DENSITIES OF ASYMMETRIC CORONAL SPECTRAL PROFILES: IMPLICATIONS FOR THE MASS SUPPLY OF THE SOLAR CORONA
12. CAN THE DIFFERENTIAL EMISSION MEASURE CONSTRAIN THE TIMESCALE OF ENERGY DEPOSITION IN THE CORONA?
13. DIAGNOSING THE TIME DEPENDENCE OF ACTIVE REGION CORE HEATING FROM THE EMISSION MEASURE. II. NANOFLARE TRAINS
14. DIAGNOSING THE TIME-DEPENDENCE OF ACTIVE REGION CORE HEATING FROM THE EMISSION MEASURE. I. LOW-FREQUENCY NANOFLARES
15. ENTHALPY-BASED THERMAL EVOLUTION OF LOOPS. III. COMPARISON OF ZERO-DIMENSIONAL MODELS
16. ENTHALPY-BASED THERMAL EVOLUTION OF LOOPS. II. IMPROVEMENTS TO THE MODEL
17. WHAT DOMINATES THE CORONAL EMISSION SPECTRUM DURING THE CYCLE OF IMPULSIVE HEATING AND COOLING?
18. ON THE ISOTHERMALITY OF SOLAR PLASMAS
19. A SIMPLE MODEL FOR THE EVOLUTION OF MULTI-STRANDED CORONAL LOOPS
20. EXPLOSIVE INSTABILITY AND CORONAL HEATING
21. SPECTROSCOPIC OBSERVATIONS OF HOT LINES CONSTRAINING CORONAL HEATING IN SOLAR ACTIVE REGIONS
22. HINODE X-RAY TELESCOPE DETECTION OF HOT EMISSION FROM QUIESCENT ACTIVE REGIONS: A NANOFLARE SIGNATURE?
23. Static and Impulsive Models of Solar Active Regions
24. Highly Efficient Modeling of Dynamic Coronal Loops
25. Are Constant Loop Widths an Artifact of the Background and the Spatial Resolution?
26. The Cross‐Field Thermal Structure of Coronal Loops from Triple‐FilterTRACEObservations
27. The Temporal Evolution of Coronal Loops Observed byGOESSXI
28. Nonthermal Spectral Line Broadening and the Nanoflare Model
29. The Magnetic Structure of Coronal Loops Observed byTRACE
30. The Origin of High‐Speed Motions and Threads in Prominences
31. Coronal Loop Heating by Nanoflares: The Impact of the Field‐aligned Distribution of the Heating on Loop Observations
32. An Explanation for the “Switch‐On” Nature of Magnetic Energy Release and Its Application to Coronal Heating
33. Coronal Seismology and the Propagation of Acoustic Waves along Coronal Loops
34. A Model for Bright Extreme‐Ultraviolet Knots in Solar Flare Loops
35. The Inability of Steady‐Flow Models to Explain the Extreme‐Ultraviolet Coronal Loops
36. Constraints on the Magnetic Field Geometry in Prominences
37. The Long‐Term Evolution of AR 7978: Testing Coronal Heating Models
38. The Long‐Term Evolution of AR 7978: The Scalings of the Coronal Plasma Parameters with the Mean Photospheric Magnetic Field
39. A Transient Heating Model for Coronal Structure and Dynamics
40. Spectroscopic Diagnostics of Nanoflare‐heated Loops
41. Are Magnetic Dips Necessary for Prominence Formation?
42. Twisted Coronal Magnetic Loops
43. Three‐dimensional Stereoscopic Analysis of Solar Active Region Loops. II.SOHO/EIT Observations at Temperatures of 1.5–2.5 MK
44. Magnetic Field and Plasma Scaling Laws: Their Implications for Coronal Heating Models
45. Three‐dimensional Stereoscopic Analysis of Solar Active Region Loops. I.SOHO/EIT Observations at Temperatures of (1.0–1.5) x 106K
46. The Dynamic Formation of Prominence Condensations
47. A Model for Solar Coronal Mass Ejections
48. A Self‐consistent Model for the Resonant Heating of Coronal Loops: The Effects of Coupling with the Chromosphere
49. A Nanoflare Explanation for the Heating of Coronal Loops Observed byYohkoh
50. The Occurrence Rate of Soft X‐Ray Flares as a Function of Solar Activity
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