DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 1
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | EP DRA | 286.7359 | 69.1573 | 286.793684 | 69.076999 | 30.014466 | 83.210835 | 100.08892772 | 23.87463538 | 44.5637 | 57164.4409953704 | 2015-05-22 10:35:02 | 57166.2856365741 | 2015-05-24 06:51:19 | 410006010 | 80.2346 | 80 | 80.2346 | 80.2426 | 0 | 80.2426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.9585 | 67.9585 | 155.5819 | 1 | PROCESSED | 57618.7517939815 | 2016-08-18 18:02:35 | 57558 | 2016-06-19 00:00:00 | 57176.3159027778 | 2015-06-03 07:34:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100018 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 10 | AO10 | CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/ | Quick Look |
Used SQL
SELECT * FROM suzaku_master_data WHERE observation_id = '410006010'
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