1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
What Are You Looking at?
Jerry Gilfoyle The Zeeman Effect 1 / 17 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
What Are You Looking at?
1 Hint: It makes these happen.
Jerry Gilfoyle The Zeeman Effect 1 / 17 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
What Are You Looking at?
1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO).
Jerry Gilfoyle The Zeeman Effect 1 / 17 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
What Are You Looking at?
1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite.
Jerry Gilfoyle The Zeeman Effect 1 / 17 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
What Are You Looking at?
1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss.
Jerry Gilfoyle The Zeeman Effect 1 / 17 6 Why should you care? Ask him.
What Are You Looking at?
1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather.
Jerry Gilfoyle The Zeeman Effect 1 / 17 What Are You Looking at?
1 Hint: It makes these happen. 2 This a magnetogram from the Solar Dynamics Observatory (SDO). 3 It shows the magnetic field strength and polarity along the line of sight from the satellite. 4 The legend shows the field strength in gauss. 5 Understanding the Sun’s magnetic field is essential for understanding solar weather. 6 Why should you care? Ask him.
Jerry Gilfoyle The Zeeman Effect 1 / 17 1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
Jerry Gilfoyle The Zeeman Effect 2 / 17 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements.
Jerry Gilfoyle The Zeeman Effect 2 / 17 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy.
Jerry Gilfoyle The Zeeman Effect 2 / 17 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot.
Jerry Gilfoyle The Zeeman Effect 2 / 17 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides.
Jerry Gilfoyle The Zeeman Effect 2 / 17 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region.
Jerry Gilfoyle The Zeeman Effect 2 / 17 The Zeeman Effect!
How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
Jerry Gilfoyle The Zeeman Effect 2 / 17 How Do We Measure the Magnetic Field on the Surface of the Sun?
1 The Sun consists of hydrogen (71.0%), helium (27.1%) and 65 other elements. 2 These atoms are constantly absorbing and emitting energy. 3 Left-hand side shows close-up of a sunspot. 4 Right-hand side shows spectroscopic lines. One of the lines divides. 5 The split lines are caused by the high magnetic field in that region. 6 The splitting of spectroscopic lines was first observed by Pieter Zeeman (Nobel with Lorentz in 1902).
The Zeeman Effect!
Jerry Gilfoyle The Zeeman Effect 2 / 17 The Question
Left-hand plot below shows spectra of a sunspot. The labels from (A) to (D) correspond to the locations indicated in right-hand image. The single line (A) is split as the position shifts into the sunspot. The absorption lines at 6301.5 angstroms and 6302.5 angstroms are from iron. What is the size of the magnetic field that created the observed splitting?
Jerry Gilfoyle The Zeeman Effect 3 / 17 Hydrogen Eigenvalues (Energy Levels)
5 µ(e2)2 13.6 eV En = − 2 2 = − 2 Continuum 2~ n n States
0
Discrete States
-5 Energy ( eV )
-10
-15 0 2 4 6 8
Jerry Gilfoyle The Zeeman Effect 4 / 17 Hydrogen Eigenvalues (Energy Levels)
5 µ(e2)2 13.6 eV En = − 2 2 = − 2 Continuum 2~ n n States
0
Discrete States
-5 Energy ( eV )
-10
-15 0 2 4 6 8
Jerry Gilfoyle The Zeeman Effect 4 / 17 Zeeman Effect - Hα line in hydrogen
Jerry Gilfoyle The Zeeman Effect 5 / 17 Current Loop in a Magnetic Field - 1
B z I
p r
Jerry Gilfoyle The Zeeman Effect 6 / 17 Current Loop in a Magnetic Field - 2
B
I in µ F θ in
τ in
z Fout
I out y x out Jerry Gilfoyle The Zeeman Effect 7 / 17 Current Loop in a Magnetic Field - 3
B
I in µ F θ in
τ in
z Fout
I out y x out Jerry Gilfoyle The Zeeman Effect 8 / 17 Current Loop in a Magnetic Field - 4
Jerry Gilfoyle The Zeeman Effect 9 / 17 Current Loop in a Magnetic Field - 5
Jerry Gilfoyle The Zeeman Effect 10 / 17 Current Loop in a Magnetic Field - 6
Jerry Gilfoyle The Zeeman Effect 11 / 17 Current Loop in a Magnetic Field - 6
Jerry Gilfoyle The Zeeman Effect 11 / 17 Current Loop in a Magnetic Field - 7
B
µ
θ
I out I in
Fout Fin
z
y x out Jerry Gilfoyle The Zeeman Effect 13 / 17 Current Loop in a Magnetic Field - 8
B
I in µ F θ in
τ in
z Fout
I out y x out Jerry Gilfoyle The Zeeman Effect 14 / 17 Current Loop in a Magnetic Field - 8
B
I in µ F θ in
τ in
z Fout
I out y x out Jerry Gilfoyle The Zeeman Effect 15 / 17 Test the Model - Zeeman Effect and Hα line in hydrogen
Jerry Gilfoyle The Zeeman Effect 16 / 17 The Question
Left-hand plot below shows spectra of a sunspot. The labels from (A) to (D) correspond to the locations indicated in right-hand image. The single line (A) is split as the position shifts into the sunspot. The absorption lines at 6301.5 angstroms and 6302.5 angstroms are from iron. What is the size of the magnetic field that created the observed splitting?
Jerry Gilfoyle The Zeeman Effect 17 / 17