Transcript – a common Rydberg Matter form of matter in the Universe Leif Holmlid

Rydberg Matter – a common
form of matter in the Universe
Leif Holmlid
Abstract:
The electronically excited condensed matter named Rydberg Matter seems
to be a state of matter of the same significance as liquid or solid matter. In
fact, it may be the most common form of matter in the Universe. In this talk,
spectroscopic signatures from space will be discussed and described in
terms of transitions in Rydberg Matter, both in emission, absorption, and
stimulated Raman. The interpretations are based on experimental results.
Recent experiments give proof for metallic atomic hydrogen, of interest not
only for intergalactic space but possibly also for understanding planets like
Jupiter.
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Rydberg Matter forms planar clusters
Core ions
QM allowed region for
RM electrons
A perspective view of
a cluster of Rydberg
Matter with 19 atoms
or molecules. The
core ions in space will
in general be H+ and
H2+, with one electron
per atom or molecule
excited to the RM
region. The clusters
are formed by
interacting circular
Rydberg species
Classical orbiting RM electrons
High Rydberg electron
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Experimental verification: RM in a tunable cavity - the RM laser
The RM laser is a thermal laser, converting thermal energy to laser light in the IR.
Extremely broadband tunable, 800 – 16000 nm and longer.
MCT detector
Vacuum chamber
Chopper
Grating
RM medium
Windows
Publications on stimulated emission from RM:
L. Holmlid, Chem. Phys. Lett. 367 (2003) 556-560.
S. Badiei and L. Holmlid, Chem. Phys. Lett. 376 (2003) 812-817.
L. Holmlid, J. Phys. B: At. Mol. Opt. Phys. 37 (2004) 357-374.
Atmospheric Science
Schematical
drawing of the
setup for
observing the
spectra of
stimulated
emission. The
grating is turned
under computer
control. The
chopper and end
mirror can be
replaced by a
spinning mirror.
Emitters for RM: here alkali doped metal oxide
catalysts, otherwise carbon w. alkali atoms
GÖTEBORG UNIVERSITY
Chemistry
Metal-like conduction band
with delocalized electrons that give the bonding
e-
Transitions
for the
stimulated
emission
Rydberg Matter states
e
-
Rydberg
levels
Low core electrons
K
Two-electron processes in general
K
K*
KN* (RM)
Stimulated emission
hn
Thermal
desorption
Energy diagram for RM
Re-excitation
K(nlm)
K(4S1/2 )
K (adsorbed)
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Stimulated emission: signal from cavity
40
Intensity (arb. units)
17
30
n2 = 40-80
n4" =
20
14
10+11
13
10
15
16
n4”
Concave mirror
12
Plane mirror
0
2000
4000
6000
8000
Wavelength (nm)
Cutoff due to MCT detector
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Stimulated emission from RM
n2
n4”
RM theory agrees well with UIR bands: A&A 358 (2000) 276-286
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
UIR band structure:
Stimulated Raman with He-Ne laser, backscattered
Calculated from Raman shift
Signal
Signal
Measured
55
10
10
Converted wavelength (mm)
Type A
Type B
objects
10
Wavelength (mm)
Signal
objects
Signal
Astrophys. J. 548
(2001) L249-L252.
13
UIR type A = nebulae, galaxies
Bregman et al. (1989)
Atmospheric Science
Black curves:
calculated from
RM model to fit
Type B
Type A
5
Converted
wavelength ( mm)
5
10
Wavelength (m m)
15
UIR type B = carbon-rich stars
Buss et al. (1993)
GÖTEBORG UNIVERSITY
Chemistry
Peaks of unidentified infrared bands = UIR bands
High upper level due to resonance with
Rydberg state stimulated emission
n = 9 5 and 7 5.
Observations
80
80
Upper level n2 at peak
Upper level n2 at peak
90
70
60
50
40
30
20
Experiments
60
40
20
0
10
12
14
16
18
20
22
Lower level n4"
24
26
28
8
10
12
14
16
18
20
22
Lower level n4"
Comparison of transitions in the RM laser and in
space (from Kahanpää et al. 2003)
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Diffuse interstellar bands (DIBs)
seen in absorption against reddened stars
More than 280 bands with widths 0.5 – 140 cm-1 at 400 -900 nm
Process for DIB transitions:
RM states
n=
6
4
5
Ion in
RM
Ion in
RM
Process 64
co-planar state
n3
n4
R 4R 5
L. Holmlid, “Rydberg Matter as the diffuse interstellar band (DIB) carriers in interstellar space:
the model and accurate calculations of band centers”.
Phys. Chem. Chem. Phys. 6 (2004) 2048-2058.
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
DIB band heads
Table 4: Calculat ed DIB band head posit ions for t ransit ions t o coplanar circular Rydberg at oms wit h t he
innermost elect ron at n = 1. No correct ions are made t o ¯t t he observed bands. T he Rydberg const ant used
for each band is shown in t he t hird column. W indicat es t he equivalent widt h of t he band. An overlap ol is
indicat ed wit h ot her bands. Probable in t he last column means t hat unassigned peaks in t he spect ra in Ref. [4]
overlap.
Transit ion
71 Ã R4 R1
61 Ã R4 R1
51 Ã R4 R1
121 Ã R5 R1
111 Ã R5 R1
101 Ã R5 R1
91 Ã R5 R1
81 Ã R5 R1
71 Ã R5 R1
Calculat ed
º~ (cm¡ 1 )
25194.9
24386.3
23045.7
16791.1
16646.3
16455.8
16203.1
15843.3
15318.5
R( )
1
1
1
H2
H2
H2
1
1
1
¢ º~
76
Observed
º~ (cm¡ 1 )
25118.5
FWHM
(cm¡ 1 )
126.3
14
16632.7
9.7
19
12
14
16183.8
15830.9
15304.8
60.3
53.2
39.8
Wavelengt h ( ºA )
3980
4099.5
4338.0
5953.9
6010.6
6072.0
6177.3
6315.0
6532.1
W ( ºA )
Overlap
-
ol
ol HI O
ol HI O
probable
0.141
ol NeI HeI
0.773
0.352
0.664
18
Phys. Chem. Chem. Phys. 6 (2004) 2048-2058.
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Best evidence: 60 sharp DIB bands
Table 7: Assignment s of DIB bands in a range around 6000 ºA . All observed bands from t he DIB dat abase [6]
in t his range are included. See furt her t he t ables above. (o) means probable according t o Ref. [6].
WaveW ( ºA )
º
lengt h ( A )
5809.1
0.016
5810.0
0.037
5814.3 (o) 0.004
5818.6
0.004
5828.5
0.003
5837.9
0.001
5840.7
0.003
5842.1
0.005
5842.7 (o) 0.002
5843.4
0.004
5844.5
0.077
5844.8
0.009
5845.4 (o) 0.004
5847.7 (o) 0.002
5849.8
0.048
5850.2
0.006
5900.6
0.013
5902.8 (o) 0.007
5904.6
0.009
5908.3 (o) 0.003
5910.7
0.015
5923.4
0.027
5925.9
0.015
5927.5 (o) 0.011
5929.6 (o) 0.007
5945.2
0.013
5947.3
0.017
5948.9
0.005
5975.6
0.006
5982.5
0.015
5986.4
0.008
5988.0
0.012
5995.8
0.012
Atmospheric
Science
5999.8
0.006
FWHM
(cm¡ 1 )
3.3
7.4
1.2
1.4
0.9
1.5
1.5
0.7
2.3
2.3
8.8
1.4
2.0
1.8
2.9
4.4
2.0
3.4
2.0
3.4
2.6
1.7
2.8
2.0
1.7
1.7
2.8
1.7
2.2
2.8
2.5
3.1
3.3
1.7
Observed
º~ (cm¡ 1 )
17209.6
17206.9
17194.2
17181.5
17152.3
17124.7
17116.5
17112.4
17110.6
17108.6
17105.4
17104.5
17102.7
17096.0
17089.9
17088.7
16942.7
16936.4
16931.3
16920.7
16913.8
16877.5
16870.4
16865.8
16859.9
16815.6
16809.7
16805.2
16730.1
16710.8
16699.9
16695.4
16673.7
16662.6
¢ º~
Calculat ed
º~ (cm¡ 1 )
Transit ions
0
0
0
1
0
2
17206.7
17193.9
17181.6
17153.4
17124.5
17118.2
1716 Ã R16 R5
1714 Ã R14 R5
1711 Ã R11 R5 ;
1614 Ã R14 R5
161 Ã R1 R5
1515 Ã R15 R5
-2
17106.9
1514 Ã R14 R5
1
17105.2
1417 Ã R17 R5
1
-1
-2
0
-3
0
1
2
17097.2
17089.0
17086.8
16942.5
16933.9
16930.9
16921.9
16915.3
1513 Ã R13 R5
1512 Ã R12 R5
1416 Ã R16 R5
1311 Ã R11 R5
1116 Ã R16 R5
1310 Ã R10 R5
139 Ã R9 R5
138 Ã R8 R5
3
16873.5
1212 Ã R12 R5
7
-2
0
-3
16853.0
16813.8
16809.4
16802.0
1114 Ã R14 R5 ;
1113 Ã R13 R5
128 Ã R8 R5
127 Ã R7 R5
1211 Ã R11 R5
6
16716.4
1110 Ã R10 R5 ;
1013 Ã R13 R5
-2
3
2
16693.9
16676.7
16664.4
119 Ã R9 R5
118 Ã R8 R5
117 Ã R7 R5
1617 Ã R17 R5
GÖTEBORG UNIVERSITY
Chemistry
Intensities for all DIBs
X overlap with
other transitions
Band heads
Figure 4: T he int ensity dist ribut ion of t he DIBs arranged according t o t he ¯nal st at e in a t ransit ion (n 4 ) n 3 Ã
R5 Rn 3 . T he int ensity is summed for t he di®erent Rydberg const ant component s and given as t he equivalent
widt h (see t he Tables). Crosses means t hat ot her t ransit ions overlap, and t he t hick black line indicat es t he
cases of t ransit ions wit h low int ensity t o st at es (n) n .
Low intensity for
states nn
n4-1
Phys. Chem. Chem. Phys. 6 (2004) 2048-2058.
25
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
DARK MATTER = RM?
H atom in RM with n=80 occupies
1012 larger volume than in ground state..
Badiei & Holmlid, “Rydberg
Matter in space - low density
condensed dark matter”.
Mon. Not. R. Astron. Soc.
333 (2002) 360-364.
Stack of RM clusters,
stable at low temperature.
Attracted and aligned by
magnetic forces, held apart
by electrostatic forces
Faraday rotation in intergalactic space
Badiei & Holmlid, “Magnetic
field in the intracluster medium:
Rydberg matter with almost free
electrons”.
Mon. Not. R. Astron. Soc. 335
(2002) L94-L98.
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Quantized redshifts
at 21 cm wavelength
Observed in the local
supercluster of galaxies
Ionization limit
Atomic states
Atmospheric Science
Translating states
Bonding
RM electrons
Redshift from
stimulated Raman
in translating electron
states in RM clusters
Astrophys. Space Sci.
291 (2004) 99-111
GÖTEBORG UNIVERSITY
Chemistry
Vacuum
chamber
Experimental studies
of redshifts in RM
Cryostat
20-60 K
Lead salt
diode lasers
single-mode
Dn = 10-4 cm-1
Chopper
and
focusing
Emitter
with RM cloud
Parallel beam
Appl. Phys. B 79 (2004) 871-877.
Similar studies:
Phys. Rev. A 63 (2001) 013817-1-013817-10.
Eur. Phys. J. Appl. Phys. 26 (2004) 103-111.
Atmospheric Science
Water cooled
isolated box
Fabry-Perot
interferometer
MCT
detector
GÖTEBORG UNIVERSITY
Chemistry
RM emitter temp.
Redshifts in
transmission
through cold RM
h:min
6
+0.53
5:50
+0.48
4:17
5
+0.44
Size 0.02
cm-1
Signal (arb. units)
3:21
+0.34
2:27
4
+0.34
2:22
+0.24
1:53
3
+0.24
300 K
1:47
+0.17
1:19
2
+0.12
1:02
+0.08
0:46
1
0:08
1200 K
+0.01
0
300 K
11.27
0
o
T ( C)
200
300
400
500
Etalon
temperature
T coeff.
10-2
cm-1 K-1
600
Laser current (mA)
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
0.3
Redshifts 0.02 cm-1 in reflection
from deposited (cold) layer of RM
Difference
0.2
0.1
Hot RM gives blueshifts instead.
0.0
-0.1
-0.2
Signal (arb. units)
2.0
-0.3
Redshifts in space
1.5
1.0
Calculations using stimulated
Raman theory from these
results give redshifts of at
least the same size as
observed
1200 K
0.5
0.0
300 K
-0.5
250
300
350
400
450
500
Laser current (mA)
Appl. Phys. B 79 (2004) 871-877
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Pulsed laser fragmentation of RM
ns pulses excite pairs of electrons and
give Coulomb explosions.
The smaller cluster/ particle moves away
with most of the kinetic energy
d = 2.9 n2 a0
Excitation levels in RM, with energy release W.
W=
e2/(4pe
0d)
Excitation level n
1
2
3
4
5
6
7
Energy release W (eV)
9.38
2.35
1.04 0.59 0.38 0.26 0.19
Interionic distance d (nm) 0.153 0.614 1.38 2.46 3.84 5.53 7.52
Low excitation levels in RM are studied
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Hydrogen molecule RM
RM Coulomb explosion
experiments
37
15000
12000
1
Counts
Rydberg Matter
cloud
Emitter
Laser beam
N=
61 91
7 19
(H2)N*
9000
6000
Rotation center
90 mm
3000
14
o
0
Detector at 0
1
o
Wang & Holmlid, Chem. Phys. Lett. 325 (2000) 264-268,
Chem. Phys. 261 (2000) 481-48, ibid 277 (2002) 201-210;
Badiei & Holmlid Int. J. Mass Spectrom. 220 (2002) 127-136,
Chem. Phys. 282 (2002) 137-146.
Calc. signal
Detector at 55
7
37
n=3
61 91
19
0
50
1.04 eV
100
150
Time-of-flight (ms)
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Hydrogen atom RM at n = 1
9.4 eV from
Coulomb explosion
d = 150 ± 8 pm
6000
H*
(n = 3)
*
H (2+)
(n = 1)
(H2) 7-14 (n = 3)
*
H
(n = 1)
H* (3+)
(n = 1)
4000
*
H2* (n = 3)
5000
Signal (counts)
Signal (counts)
5000
n = 1 is the lowest possible
state of RM which is
the same as metallic hydrogen
-10 V
3000
0V
2000
+5 V
4000
-10 V
3000
0V
2000
+5 V
1000
1000
(H2*)7
+10 V
0
+
+10 V
0
0
1
2
3
4
5
Time-of-flight (ms)
6
0
10
20
30
40
50
Time-of-flight (ms)
Badiei & Holmlid, Phys. Lett. A 327 (2004) 186-191
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
Multiple repulsions + <--> 2+ (18 ev), 3+ (27 eV)
Very high proton
energies
14000
12000
50
10000
40
8000
30
6000
20
4000
H2
n = 3, 4
2000
0
0
2
4
6
8
10
Ang le (deg rees)
Cosmic rays?
16000
S ig n a l (co u n ts)
Hydrodynamic
acceleration
> 1 keV for H+
observed in
experiments with
acceleration
lengths of 1 cm
H
n=1
0
10
12
14
Time-of-flig ht ( ms)
Badiei & Holmlid, J. Phys.: Condens. Matter 16 (2004) 7017-7023.
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
IR observation from comets
Ultra-red matter detected might be RM.
RM emits selectively in the IR, as seen
in the RM laser
”Deep Space” flyby at Comet 19P/Borrelly
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry
a)
b)
Polarization at comets
Reflectance of sun from comets,
visible light, unpolarized
Negative polarization possible?
Polarization P (%)
30
from Sun
from Sun
Theoretical
for RM
20
two classes
10
The observed polarization P
is much too low for almost any
assumption about particle size,
shape and composition.
Planar RM clusters probably
have few polarizability
elements (but large!)
which gives good agreement.
0
Phase angle (degrees)
Atmospheric Science
GÖTEBORG UNIVERSITY
Chemistry